1000 Sentences With "giant star" | Random Sentence Generator

So you're a giant star that many people have not heard of. Yeah.

Artist's depiction of a white dwarf (right) in orbit around a white giant star.

The red giant star is 35,000 light-years from Earth, in the Milky Way's halo.

The hourglass-shaped nebula is due to an aging red giant star and a white dwarf.

The red super-giant star Betelgeuse has dramatically dimmed, leading to speculation of an imminent supernova.

Within it, two giant star clusters appear brilliant white and are swaddled by greenish hydrogen gas clouds.

Over its short life of a few million years, the giant star lost 85% of its mass.

Robin Williams was a giant star because he was this manic, joyful, mile-a-minute funny person. Right?

He's a giant star; he didn't need to be on the social media platform in the first place.

Essentially, the binary consists of a dying old red giant star that has expelled its outer layer as stellar wind.

Exhibit A: The Witch Head Nebula, located 133 light years from Earth and illuminated by the nearby giant star Rigel.

There's also giant Star Destroyers, Ben Mendelsohn, the Death Star, lots of war action, and a foreboding sense of dread.

That said, Earth will be inhospitable by that time due to the expansion of the Sun into a red giant star.

NGC 26 is a planetary nebula, and at its center is a dying red giant star surrounded by a ring of gas.

They're formed when a giant star collapses, imploding into a tiny area of such intense gravity, even the surrounding light is sucked in.

It's not hard to imagine James potentially running the international businesses that come with the deal: Satellite service Sky and Indian media giant Star.

That&aposs why many people are excited that Betelgeuse, a bright red super giant star in the constellation Orion, has suddenly and dramatically dimmed.

Their efforts paid off -- they soon spotted a giant star eight times heavier than the sun, orbiting around what turned out to be LB-1.

Then they need to find a way to stop that force from escaping and hurting anybody else — especially a giant star base within easy striking distance.

The two black holes that sent out ripples in space and time as they merged were born in the belly of a giant star, new research suggests.

"With detailed images of the environment of HD101584 we can make the connection between the giant star it was before, and the stellar remnant it will soon become."

Perfect for when you're out and about, this solar charger converts energy from that giant star in the sky, delivering enough juice to power two devices at once.

With detailed images of the environment of HD101584 we can make the connection between the giant star it was before, and the stellar remnant it will soon become.

Lensing occurs when a large object, such as a giant star or galaxy cluster, passes in front of more distant background objects, from our point of view on Earth.

I honestly felt as if "Giant star?" at 1016630D was going to be a veiled capital clue that revealed a football player, but that was me overthinking things again.

Astronomers think Betelgeuse&aposs dimming is most likely just another short phase in the life of a giant star that&aposs burning through the last dregs of its fuel.

It'll burn for another 5 billion years before it will have fully exploded into a red giant star, expanding as far as Mars and destroying everything humans have ever touched.

You had a set number of "lives" to get through each level, but once you committed to these giant Star Wars dioramas, you had to finish the level in a single session.

But according to Yesterland, a blog about retired Disney attractions, the Streets of America closed for good on April 2, 2016, and has since been replaced by the giant Star Wars: Galaxy's Edge land.

This suggests that this extrasolar system formed from a cloud of material that was enriched by a supernova , or the death of a giant star called an asymptotic giant branch (AGB) star, the researchers said.

As the nation's capital prepares for the massive snowstorm headed its way this week, the Washington D.C. Snowball Fight Association has scheduled a giant Star Wars-themed snowball fight for Saturday at Dupont Circle Fountain.

The DivineBy Asaf Hanuka, Tomer Hanuka, and Boaz Lavie, published by First Second Tomer Hanuka is a giant star of illustration, and I've been watching lesser artists build careers imitating him for about a decade.

During an intramural football game at Fort Benning, Georgia, the Army band honored their interfaith efforts by forming a giant Star of David and playing "Ein Keloheinu," an ancient Jewish prayer about the uniqueness of God.

In about five billion years, when the Sun enters old age as a red giant star, the Moon's orbit will be about 40 percent wider than it is now, and Earth's day may last over 40 hours.

The industry still isn't back to where it was at its 1999-ish peak, when Britney Spears was a giant star and people bought CDs for $15, even if they only wanted to hear a single song.

I was surprised to remember, because you reminded me, that he was a giant star in the '70s, early '80s as a stand-up and on TV, and then was not a movie star for a long time.

"This is the first time that we have such a giant star that is unambiguously imaged with that level of detail," said Fabien Baron, assistant professor in the Department of Physics and Astronomy at Georgia State University, in a statement.

Ms. James, who often presides over Council meetings seated in a red and white upholstered chair marked with a giant star, has also used the public advocate's office to introduce 48 pieces of legislation, 10 of which are now law.

Click here to view original GIFInstead of sticking his camera's lens in the eyepiece of a powerful telescope peering into the heavens, filmmaker Thomas Vanz captured this stunning footage of a giant star going all supernova by actually pointing his camera at a glass aquarium filled with colorful inks and water.

HD 128198 is a giant star in the northern constellation of Boötes.

HD 134335 is a giant star in the northern constellation of Boötes.

Gamma Boötis presents as an A-type giant star belonging to spectral class A7III.

HD 27245 is a variable red giant star in the northern constellation of Camelopardalis.

Giant star, entry in Cambridge Dictionary of Astronomy, Jacqueline Mitton, Cambridge: Cambridge University Press, 2001. .

The visible member of this inner pair is an aging giant star with a stellar classification of K4III.

It was later resolved into an O3.5 supergiant spectroscopic binary and an O4 giant star separated by approximately 500 AU.

Sigma Aurigae, Latinized from σ Aurigae, is a giant star in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 4.99. With an annual parallax shift of 6.21 mas, it is approximately distant from the Earth. This is an evolved giant star with a stellar classification of K4 III.

HD 199442 is a giant star situated in the Aquarius constellation. It is located about 310 light years from the solar system.

HD 96660 is an orange giant star located approximately 560 light years away, in the constellation Centaurus. Its apparent magnitude is 6.44.

HD 63399 is an orange giant star located approximately 445 light years away, in the constellation Puppis. Its apparent magnitude is 6.46.

Gamma Leonis b is an extrasolar planet located 125.5 light years away in the constellation Leo, orbiting the giant star Gamma Leonis.

HD 17092 b is an extrasolar planet located approximately 750 light years away in the constellation Perseus, orbiting the giant star HD 17092.

HD 34880 is a blue giant star of magnitude 6.41 in the constellation of Orion. It is 679 light years from the solar system.

IZ Aquarii is a red giant star in the constellation Aquarius. It is a slow irregular variable that varies between magnitudes 6.23 and 6.47.

HD 36678 is red giant star in the northern constellation of Auriga. It is currently on the asymptotic giant branch of the HR diagram.

41 Ursae Majoris is a red giant star in the constellation Ursa Major. It is 690 light years from Earth. The apparent magnitude is 6.34.

HD 36041 is giant star in the northern constellation Auriga. It has an apparent magnitude of 6.37, making it faintly visible to the naked eye.

HD 33463 is a suspected variable star in the northern constellation of Auriga. This is a red giant star with a stellar classification of M2III.

HD 139357 is a 6th magnitude K-type giant star located approximately 390 light years from Earth, visible in the constellation Draco. Its mass is four thirds that of our Sun but its radius is 11.47 times larger. However, despite being a giant star, it is only 3.07 billion years old, which is younger than our Sun. It hosts a planet discovered in 2009.

Astrophysicists currently calculate that in a few billion years the Earth will probably be swallowed by the expansion of the Sun into a red giant star.

La Superba (Y CVn, Y Canum Venaticorum) is a strikingly red giant star in the constellation Canes Venatici. It is a carbon star and semiregular variable.

R Aurigae (R Aur) is a M-type giant star in the constellation of Auriga. It has an apparent visual magnitude which varies between 6.7 and 13.9.

HD 102272 is a K-type giant star approximately 800 light-years away in the constellation of Leo. , two extrasolar planets are known to orbit the star.

Iota Draconis b, formally named Hypatia (pronounced or ), is an exoplanet orbiting the K-type giant star Iota Draconis about 101.2 light-years (31 parsecs, or nearly km) from Earth in the constellation Draco. The exoplanet was found by using the radial velocity method, from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star. It was the first planet discovered orbiting a giant star.

The two stars form an eclipsing binary system (variable star designation: V1488 Cyg) similar to Algol. The orbital plane of the two stars is nearly aligned with the line of sight from the Earth, so that the giant star eclipses the secondary component once per orbit. During an eclipse, emission lines can be seen in the spectrum of this system. These originate in the stellar wind escaping from the giant star.

It is drifting closer to the Earth with a heliocentric radial velocity of −14 km/s. Tokovinin (2008) catalogued this as a wide triple star system. The primary component is an aging giant star, currently in the Hertzsprung gap, with a stellar classification of . It is a weak G-band star, a luminous giant star with a carbon abundance about a factor of 5 lower than is typical for such stars.

HD 82886 is an evolved giant star in the constellation Leo Minor. With an apparent magnitude 7.63, it is too faint to be seen with the unaided eye.

HR 3830 is an orange giant star, type K0III, in the southern hemisphere constellation of Antlia. It is 311 light years from Earth. Its apparent magnitude is 5.68.

HD 220074 is a M2III red giant star located in Cassiopeia. It had been considered K1V but is now known as M2III due to radius and surface gravity.

The EG Andromedae system hosts a white dwarf and an evolved giant star, with an orbital period of 482 days and a half. The giant star is losing mass through its stellar wind at a rate higher than 10−6 /yr, and the white dwarf is accreting a fraction of this mass without forming an accretion disk. The white dwarf itself could emit a hot wind that interacts with the cooler one of the giant star, in addition to inducing the photoionization of the latter. X-ray observations, however, failed to detect emission coming from colliding winds, but established the non-magnetic nature of the white dwarf and estimated its accretion rate at 1-10 /yr.

HD 165634 is a class G7III (yellow giant) star in the constellation Sagittarius. Its apparent magnitude is 4.56 and it is approximately 339 light years away based on parallax.

HD 189831 is a class K5III (orange giant) star in the constellation Sagittarius. Its apparent magnitude is 4.77 and it is approximately 366 light years away based on parallax.

HD 18970 is a class G9.5III (yellow giant) star in the constellation Perseus. Its apparent magnitude is 4.77 and it is approximately 211 light years away based on parallax.

The giant star Antares, which is very red (spectral class M1), is surrounded by a large, red reflection nebula. Reflection nebulae may also be the site of star formation.

HD 63744 is a class K0III (orange giant) star in the constellation Puppis. Its apparent magnitude is 4.71 and it is approximately 232 light years away based on parallax.

HD 51799 is a class M1III (red giant) star in the constellation Puppis. Its apparent magnitude is 4.95 and it is approximately 860 light years away based on parallax.

HD 44131 is a class M1III (red giant) star in the constellation Orion. Its apparent magnitude is 4.91 and it is approximately 465 light years away based on parallax.

The yellow-hued primary component is an evolved K-type giant star with a stellar classification of K1 III. It is an X-ray emitter with a flux of .

HD 167818 is a class K3II (orange bright giant) star in the constellation Sagittarius. Its apparent magnitude is 4.66 and it is approximately 760 light years away based on parallax.

HD 20468 is a class K2II (orange bright giant) star in the constellation Perseus. Its apparent magnitude is 4.82 and it is approximately 1180 light years away based on parallax.

HD 61772 is a class K3II (orange bright giant) star in the constellation Puppis. Its apparent magnitude is 4.98 and it is approximately 700 light years away based on parallax.

HD 208527 is a M1III red giant star located in Pegasus. It has been considered K5V, but is now known as M1III due to radius, as well as surface gravity.

HD 164712 is a giant star in the southern constellation of Apus. It shows indications of an infrared excess, suggesting there may be a dusty disk in orbit around the star.

AG Draconis is a binary star system in the northern constellation of Draco. It consists of a giant star and a white dwarf that revolve around each other every 550 days.

HD 35519 is a giant star in the direction of open cluster Messier 38. It was once treated as a cluster member, but is now known to be a foreground object.

HD 157662 is a bright giant star in the southern constellation of Ara. It has a magnitude 10.91 companion at an angular separation of 76.4″ along a position angle of 159°.

At that distance, the visual magnitude of the star is diminished by an extinction of 0.029 due to interstellar dust. It is moving closer to the Earth with a heliocentric radial velocity of −3.6 km/s. This is an evolved giant star currently on the red giant branch with a stellar classification of K1 III/IV. The luminosity class of 'III/IV' indicates the spectrum shows a blend of features matching a subgiant and giant star.

This is an evolved K-type giant star with a stellar classification of K2.5 III. It is a Barium star, which means that, for a giant star, it displays unusually strong absorption lines of singly-ionized barium and strontium. Iota Hydrae has nearly twice the mass of the Sun and has expanded to 33 times the Sun's radius. It is around 2.5 billion years old and is spinning with a leisurely projected rotational velocity of 4.5 km/s.

The star's spectrum is unusual in that it contains very strong emission lines resulting from surrounding nebulosity. W Cygni is a semi-regular variable red giant star, 618 light-years from Earth.

HD 70555 (w Puppis) is a class K2.5II-III (orange giant) star in the constellation Puppis. Its apparent magnitude is 4.83 and it is approximately 1,010 light years away based on parallax.

The brightness of this star is diminished by 0.40 in magnitude from extinction caused by interstellar gas and dust. This is an evolved giant star with a stellar classification of K3 III.

36 Aquarii (abbreviated 36 Aqr) is a yellow giant star or subgiant star in the constellation of Aquarius. 36 Aquarii is its Flamsteed designation. It is approximately 520 light-years from Earth.

HD 59686 b is an extrasolar planet that orbits at 91.1% of distance between Earth and the Sun or 0.911 AU in a very circular orbit of the giant star HD 59686.

These are stars are the ones with the bulkiest masses that remain fully conductive, and unable to ever fuse helium, and will not form planetary nebulae, thus never entering red giant star phase.

Comparison of different spectral lines indicates that the star is a giant star and that its temperature is 16 to . The probable mass of such a star is , and certainly not less than .

G Scorpii (abbreviated G Sco), also named Fuyue, is a giant star in the constellation of Scorpius. It has an apparent magnitude of +3.19. It is approximately 126 light-years from the Sun.

Alpha Indi (α Ind, α Indi) is a third magnitude giant star in the constellation Indus, located about 98 light years from the Earth. The stellar classification of this star is K0 III-IV, so it has exhausted the hydrogen at its core and evolved away from the main sequence. It has about double the mass of the Sun and is an estimated billion years old. As a giant star it has expanded to about 12 times the radius of the Sun.

Tau3 Serpentis, Latinized from τ3 Serpentis, is a G-type giant star in the constellation of Serpens. It is approximately 410 light-years from Earth. It has an apparent visual magnitude of approximately 6.108.

The brightest star of the cluster is a K5 III giant star, with 7.1 magnitude, but its membership is questionable. One more 7.9 magnitude star is visible at the north edge of the cluster.

HD 65750, also known as V341 Carinae is a bright red giant star in the constellation Carina. It is surrounded by a prominent reflection nebula, known as IC 2220, nicknamed the Toby Jug Nebula.

The less evolved secondary, component B is likewise a giant star, having a class of A3 III. It has three times the mass of the Sun and shines with 191 times the Sun's luminosity.

HD 72561 is a star in the constellation Hydra. Its apparent magnitude is 5.867. Based on parallax, it is located about 1,600 light-years (500 parsecs) away. HD 72561 is a G-type giant star.

HD 1690 is a 9th magnitude orange giant star located approximately 2,500 light-years away in the constellation of Cetus. It is a single star, and is the host star to one known extrasolar planet.

Component A is the cool giant star, the brighter but less massive of the pair. The hotter star is sometimes listed as the primary on the basis of its stronger showing in the blended spectrum.

The visible component has a stellar classification of , displaying mixed spectral traits of an evolved subgiant and a giant star, with a strong underabundance of iron. The CN bands of this star are very weak.

HD 135438 is a K-type giant star in the northern constellation of Boötes. It has a magnitude 9.36 companion at an angular separation of 118.2″ along a position angle of 158° (as of 2012).

HD 92036 is a single star in the equatorial constellation of Hydra. Its apparent magnitude is 4.87. This is an aging red giant star on the asymptotic giant branch with a stellar classification of M1III:Ba0.5.

HD 23089 is a spectroscopic binary star in the northern constellation of Camelopardalis. The system consists of a cooler giant star and hotter main sequence companion, with the pair orbiting each other every 6,150 days.

The visible component is an evolved K-type giant star with a stellar classification of K0 III. It is a red clump star, which indicates it is generating energy through helium fusion at its core.

Red supergiants are cool and large. They have spectral types of K and M, hence surface temperatures below 4,100 K. They are typically several hundred to over a thousand times the radius of the Sun, although size is not the primary factor in a star being designated as a supergiant. A bright cool giant star can easily be larger than a hotter supergiant. For example, Alpha Herculis is classified as a giant star with a radius of while Epsilon Pegasi is a K2 supergiant of only .

78 Aquarii (abbreviated 78 Aqr) is a star in the constellation of Aquarius. 78 Aquarii is its Flamsteed designation. It is a k3iii giant star, indicating an orange to red color. Its apparent magnitude is 6.20.

N Scorpii (N Sco) is a blue giant star in the constellation Scorpius. Its apparent magnitude is 4.23. It was initially given the Bayer designation Alpha Normae by Lacaille but later moved from Norma to Scorpius.

The spectrum of this star matches a stellar classification of B5 III, with the luminosity class of III indicating that this is a giant star. It is radiating about 851 times the luminosity of the Sun.

It has sometimes been classified as a main sequence star and sometimes as a giant star. The Galactic O-Star Spectroscopic Survey has used it as the standard star for the newly created O4 subgiant spectral type.

It is an orange-hued giant star of magnitude 2.5, 72 light-years from Earth. There are several other dimmer double and binary stars in Cygnus. Mu Cygni is a binary star with an optical tertiary component.

Trumpler 27-1 is a red supergiant star that is a member of the massive, possible open cluster Trumpler-27, where a blue giant star, a yellow supergiant star , and two Wolf–Rayet stars are also located.

HD 269810 is a blue giant star in the Large Magellanic Cloud. It is one of the most massive and most luminous stars known, and one of only a handful of stars with the spectral type O2.

It is an RS Canum Venaticorum variable with a period of 19.6 days, matching the orbital period. The stellar luminosity shows indications of ellipsoidal variation, as the primary component is partly filling its Roche lobe due to gravitational interaction between the two stars. The primary component is an evolved K-type giant star with a stellar classification of K1 III. It has a relatively high rate of spin for a giant star, showing a projected rotational velocity of 26.2 km/s and a rotation period of 19.47 days.

Theta Lyrae (θ Lyr) is a star in a trinary star system, in the constellation Lyra, approximately 770 light years away from Earth. Theta Lyrae is an orange bright giant star of the spectral type K0II, which means that it possesses a surface temperature of about 5,000 kelvins, and is many times bigger and brighter, yet cooler, than the Sun. It is orbited by a subsystem composed of BD+37° 3399 and BD+37° 3399B. 10th magnitude BD+37° 3399 is a giant star with a spectral type of K2III.

Pollux , designated β Geminorum (Latinised to Beta Geminorum, abbreviated Beta Gem, β Gem), is an orange-hued evolved giant star about 34 light-years from the Sun in the constellation of Gemini. It is the brightest star in Gemini and the closest giant star to the Sun. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified. In 2006 an extrasolar planet (designated Pollux b or β Geminorum b, later named Thestias) was confirmed to be orbiting it.

The optical spectral classification of EG Andromedae is M2IIIep, the one of a cool giant star with a peculiar spectrum and strong emission lines. The white dwarf contaminates the spectrum of the giant star photoionizes the stellar wind, giving rise to the spectral peculiarities. Emission lines H-alpha and H-beta, as well as TiO and CaI ones, change in phase with the orbit. The white dwarf is best studied in the ultraviolet, where also highly ionized species sulfur, oxygen, nitrogen, carbon and phosphorus can be identified with their absorption or emission lines.

It is approximately 63 times as luminous the Sun, with a surface temperature of 5279 K. Delta Apodis is a double star, the two components of which are 103 arcseconds apart and visible through binoculars. Delta1 is a red giant star of spectral type M4III located 630 ± 30 light-years away. It is a semiregular variable that varies from magnitude +4.66 to +4.87, with pulsations of multiple periods of 68.0, 94.9 and 101.7 days. Delta2 is an orange giant star of spectral type K3III, located 550 ± 10 light-years away, with a magnitude of 5.3.

They can be separated by a aperture telescope. The pair is a source of X-ray emission with a flux of . The stellar classification of Delta1 Chamaeleontis is K0 III, which matches an evolved K-type giant star.

The primary is itself an unresolved binary with a combined stellar classification of G9 III, which matches an aging G-type giant star that has exhausted the hydrogen at its core and evolved away from the main sequence.

The companion, θ Antliae B, is a giant star with a classification of G7 III. The pair have an orbital period of 18.3 years, a significant eccentricity of 0.445, and they have an angular separation of 0.1 arcseconds.

HD 33203 is double star in the northern constellation of Auriga. It includes a bright giant star with a stellar classification of B2II. The two components have an angular separation of 1.617″ along a position angle of 222.1°.

This notation indicates the calcium K line matches an F0 star, while the hydrogen and metal lines fit an F2 star. However, Gray et al. (2001) assigned it a class of A9IIIa, matching an A-type giant star.

The giant star doesn't fill its Roche lobe but there are still large uncertainties on its mass and radius. Even the parameters of the white dwarf are not strictly constrained, but available models can give lower and upper limits.

HD 125351 or A Boötis (A Boo) is spectroscopic binary in the constellation Boötes. The system has an apparent magnitude of +4.97, with a spectrum matching a K-type giant star. It is approximately 233 light years from Earth.

HD 24480 is a double star in the northern constellation of Camelopardalis. The brighter component is a giant star with a stellar classification of K4III and an apparent magnitude of 5.20. The pair have an angular separation of 1.71″.

HR 3833 is a K-type giant star in the constellation of Antlia. It shines with a vis mag of 5.63 from a distance of 280 ly. HR 3833 is also known by its designations HD 83380 and HIP 47199.

RV Caeli is a red giant star in the constellation Caelum. Located approximately distant, Hipparcos has found it to vary between its photometric values of 6.44 and 6.56, which roughly corresponds with the magnitude as seen with the naked eye.

HD 157753 is giant star in the southern constellation of Ara. It may be an astrometric binary, and it has a faint, magnitude 13 companion at an angular separation of 31.5″ along a position angle of 356° (as of 2000).

It is moving closer to the Sun with a radial velocity of −10.6 km/s. The stellar classification of Phi Boötis is , which would suggest it is an evolving G-type star that shows spectral traits of both a subgiant and a giant star. However, Alves (2000) has it listed as a member of the so- called "red clump", indicating that it is an aging giant star that is generating energy through helium fusion at its core. The 'Fe-2' suffix notation in its class means that it displays a significant underabundance of iron in its spectrum.

It is a thick disk star with a high galactic space velocity and an orbital eccentricity of that carries it as close as to the galactic center, and as far away as . An extrasolar planet was discovered orbiting this star in 2018. This is an evolving red giant star with a stellar classification of , with the notation indicating the spectrum shows blended characteristics of a subgiant and giant star with an underabundance of iron. At the age of around 7 billion years old, it has 0.97 times the mass of the Sun but has expanded to 12 times the Sun's radius.

This is not unexpected, because the progenitors of type Ia supernovae are thought to be white dwarfs in binary systems, and observation of SN 2014J provided empirical confirmation for this. The white dwarf is much too faint to detect at the distance of M82, but its companion would have been detectable if it had been a bright evolved giant star. It will however remain too faint if it is a second white dwarf (the double degenerate Type Ia supernova path), a lower main-sequence star, or even a giant star on the fainter part of the giant sequence.

HD 82205 is a double star in the southern constellation of Antlia. However, the primary is most likely a solitary star as the other component is deemed a line of sight companion. This is a giant star with a stellar classification of K3III.

Alpha Lupi is an ageing blue giant star of spectral type B1.5 III that is 460 ± 10 light-years distant from Earth. It is a Beta Cephei variable, pulsating in brightness by 0.03 of a magnitude every 7 hours and 6 minutes.

It appears to be slightly hotter and slightly less luminous than the inner giant star, but the exact properties are difficult to determine due to its rapid rotation, the weak absorption lines, and the presence of strong emission lines from the disk.

HD 130084, also known as HR 5510, is a variable red giant star in the constellation Boötes. Located around 810 light-years distant, it shines with a luminosity approximately 569 times that of the Sun and has a surface temperature of 3854 K.

One way to gain the additional mass would be by accreting gas from a giant star (or even main sequence) companion. A second and apparently more common mechanism to generate the same type of explosion is the merger of two white dwarfs.

To date, no outburst has been observed in EG Andromedae. The observed variability is well described by the two components eclipsing each other during the orbit. However, there is some evidence that the giant star and the wind flow have an intrinsic variation.

Alphard , designated Alpha Hydrae (α Hydrae, abbreviated Alpha Hya, α Hya), is the brightest star in the constellation of Hydra. It is a single giant star, cooler than the sun but larger and more luminous. It is about 177 light years away.

Tau6 Serpentis, Latinized from τ6 Serpentis, is a G-type giant star in the constellation of Serpens, approximately 450 light-years from the Earth. It has an apparent visual magnitude of approximately 6.000, and is a member of the Ursa Major Stream.

Psi2 Draconis is a solitary giant star in the northern circumpolar constellation of Draco, also designated 34 Draconis. It lies about a degree east of the brighter Psi1 Draconis. Psi2 Draconis has an apparent magnitude of 5.45. and is located around away.

Examples of non-anthropogenic risks are an asteroid impact event, a supervolcanic eruption, a lethal gamma-ray burst, a geomagnetic storm destroying electronic equipment, natural long-term climate change, hostile extraterrestrial life, or the predictable Sun transforming into a red giant star engulfing the Earth.

28 Andromedae is an A-type giant star, meaning it is colored bluish-white. Parallax estimates made by the Hipparcos spacecraft put the star at a distance of about 199 light years (61 parsecs). It is moving towards the solar system at a velocity of .

Eta Eridani (η Eridani, abbreviated Eta Eri, η Eri), officially named Azha (with a silent 'h', possibly ), is a giant star in the constellation of Eridanus. Based on parallax measurements taken during the Hipparcos mission, it is approximately 137 light-years from the Sun.

Electra , designated 17 Tauri, is a blue-white giant star in the constellation of Taurus. It is the third-brightest star in the Pleiades open star cluster (M45); the most visible stars in this group are named for the Seven Sisters of Greek mythology.

The primary component has a stellar classification of K3 III, which indicates it is a giant star that has exhausted the supply of hydrogen at its core and evolved away from the main sequence. It has the characteristic orange hue of a K-type star.

This is a list of protoplanetary nebulae. These objects represent the final stage before a planetary nebula. During this stage, the red giant star begins to slowly expel its outermost layers of material. A protoplanetary nebula usually glows with the light from its parent star.

51 Andromedae, abbreviated 51 And and formally named Nembus , is the 5th brightest star in the northern constellation of Andromeda, very slightly dimmer than the Andromeda Galaxy also being of 4th magnitude. It is an orange K-type giant star with an apparent magnitude of +3.59 and is about 169 light- years from the Earth/solar system. It is traditionally depicted as one of the two northern, far upper ends of the mythological, chained-to-the-rocks princess, the other being binary star system Gamma Andromedae. At an estimated age of 1.7 billion years, this is an evolved red giant star with a stellar classification of .

Keenan and McNeil (1989) listed a stellar classification of G7 II-III for 24 Cep, matching the spectrum of an evolved G-type star with blended features of a bright giant and a giant star. Older sources list a class of G8 III, which would suggest an ordinary giant star. At the age of 234 million years, it has an estimated 3.5 times the mass of the Sun and has expanded to about 13 times the Sun's radius. The star is radiating 199 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,023 K. These coordinates are a source of X-ray emission.

As a symbiotic star, RR Tel consists of a late-type red giant star in mutual orbit with a white dwarf, with substantial amounts of hot gas and warm dust around the two stars. The red giant is frequently referred to as a Mira, though the only real attempt at characterization of the pre-outburst system gave a different type of pulsating late-type giant star. The observed infrared colors and visible and infrared spectra features can be matched by a star of spectral type M5III. Such cool pulsating variable stars are known to produce circumstellar dust in the slow stellar winds flowing off such stars.

18 Delphini (abbreviated 18 Del), also named Musica , is a yellow giant star approximately 249 light-years from Earth in the constellation of Delphinus of the low northern hemisphere. An object believed to be an extrasolar planet (designated 18 Delphini b or Arion) orbits the star.

Beta Pegasi (β Pegasi, abbreviated Beta Peg, β Peg), formally named Scheat , is a red giant star and the second-brightest star (after Epsilon Pegasi) in the constellation of Pegasus. It forms the upper right corner of the Great Square of Pegasus, a prominent rectangular asterism.

The yellow hued magnitude 5.87 primary, component A, is an evolved G-type giant star with a stellar classification of G8 III. Its magnitude 7.61 companion, component B, is a yellow-white hued F-type main sequence/subgiant hybrid with a class of F3 IV-V.

The other bright star in Chamaeleon is Delta Chamaeleontis, a wide double star. The brighter star is Delta2 Chamaeleontis, a blue-hued star of magnitude 4.4. Delta1 Chamaeleontis, the dimmer component, is an orange-hued giant star of magnitude 5.5. They both lie about 350 light years away.

HD 187734 is double star in the equatorial constellation of Aquila. The primary is a magnitude 6.6 giant star, while the companion is a magnitude 9.4 A-type main sequence star. As of 2014, the pair had an angular separation of 5″ along a position angle of 99°.

This is an evolved giant star with a stellar classification of K3 IIIp and an estimated radius equal to 16 times the radius of the Sun. The outer envelope has an effective temperature of 4,367 K, giving it the cool orange-hued glow of a K-type star.

The primary is a red clump giant, a star on the cool end of the horizontal branch fusing helium in its core. The secondary star has begun to evolve off the main sequence; it is sometimes classified as a giant star and sometimes as a main-sequence star.

The star is sometimes described as a triple star, with a 7th magnitude companion away. This is an unrelated giant star much further away than the close pair. A fainter star separated by nearly was also been listed as a companion by Struve, again just an accidental optical association.

28 Monocerotis is a class K4III (orange giant) star in the constellation Monoceros. Its apparent magnitude is 4.69 and it is approximately 450 light years away based on parallax. It is an FK Comae Berenices variable, with a magnitude varying by 0.02 with a period of 0.21 days.

The visible component is a suspected chemically peculiar star with a stellar classification of A5 III, suggesting this is an evolved giant star. It has about 4.6 times the Sun's radius and is radiating 80 times the Sun's luminosity from its photosphere at an effective temperature of 7,888 K.

HD 93833 is a star in the constellation of Sextans. Its apparent magnitude is 5.842, but interstellar dust makes it appear 0.202 magnitudes dimmer than it should be. It is located some 340 light-years (104 parsecs) away, based on parallax. HD 93833 is a K-type giant star.

Many of the well-known bright stars are red giants, because they are luminous and moderately common. The red-giant branch variable star Gamma Crucis is the nearest M-class giant star at 88 light-years. The K0 red-giant branch star Arcturus is 36 light-years away.

Delta Trianguli Australis (δ TrA, δ Trianguli Australis) is a single, yellow- hued star in the constellation Triangulum Australe. It is approximately 606 light years (182 parsecs) from Earth. This is a G-type giant star with a stellar classification of G5II and an apparent magnitude of +3.86.

This is a K-type giant star with a stellar classification of K1III: − the colon suffix indicates some uncertainty in the luminosity classification of III. Spectroscopic analysis of the star was used to derive an estimated mass of about 1.81 times the mass of the Sun. It has an estimated age of 1.6 billion years; old enough at that mass to have evolved off the main sequence. As a giant star, the atmosphere has expanded to 7.3 times the Sun's radius, and it is emitting 26 times the solar luminosity at an effective temperature of 4,772 K. The projected rotational velocity of the star is 4.3 km/s, indicating it is rotating with a period of under 86 days.

Follow up observations led to the determination that it had a nearly circular orbit with a period of 5.6 days. The visible component is a chemically peculiar mercury-manganese star with a stellar classification of B9pHgMn. Other analyses of its spectrum have assigned it the giant star spectral type of B9III.

28 Aurigae (28 Aur) is a star in the constellation Auriga. Its apparent magnitude is 6.80. It is a giant star which has exhausted its core hydrogen and expanded to ten times the size of the Sun. Despite being slightly cooler than the sun at it is 73 times more luminous.

M Puppis (M Pup, HR 2789, HD 57197) is a blue giant or bright giant star (spectral type B8II/III) in the constellation Puppis. Its apparent magnitude is 5.84, which means it is visible with the naked eye under optimal conditions. It is approximately 590 light years away based on parallax.

14 Aquarii (abbreviated 14 Aqr) is red giant star. 14 Aquarii is the Flamsteed designation; it also bears the variable star designation IW Aquarii. It is a semiregular variable with an amplitude of less than a tenth of a magnitude, and shows variations on a timescale of just one day.

The primary component of is a magnitude 6.47 giant star with a stellar classification of G8 III:. A companion star at an angular separation of 1.437 arcseconds is an A-type main sequence star with a classification of A1 V. It is slightly fainter, with an apparent magnitude of 6.75.

It has an absolute magnitude of 0.12. This object is an aging giant star with a stellar classification of K2 III. With the supply of hydrogen exhausted at its core, the star has cooled and expanded off the main sequence. At present it has 20 times the radius of the Sun.

HD 178233 is a 6th magnitude star in the constellation Lyra, approximately 133 light years from Earth. It is a white giant star of the spectral type F0III, meaning it possesses a surface temperature of 6,000 to 7,500 kelvins. It is hotter, much bigger, and much brighter than our Sun.

The combined spectrum of Psi2 Orionis matches that of a B-type subgiant star with a stellar classification of B2 IV. The primary component is an evolved giant star with a class of B1 III, while the secondary is a B-type main sequence star with a classification of B2 V.

The planetary companion discovered in 2002 was the first planet known to orbit a giant star. The habitable zone for this star lies in the range of 6.8–13.5 Astronomical Units, placing this planet well inside. The alignment of this planet's orbit may make it directly detectable via the transit method.

Beta Cassiopeiae (β Cassiopeiae, abbreviated Beta Cas or β Cas), officially named Caph , is a Delta Scuti variable star in the constellation of Cassiopeia. It is a giant star belonging to the spectral class F2. The white star of second magnitude (+2.27 mag) has an absolute magnitude of +1.16 mag.

HD 95808 is a double star in the constellation of Crater. Its apparent magnitude is 5.50, but interstellar dust makes it appear 0.11 magnitudes dimmer than it should be. It is located some 340 light-years (104 parsecs) away, based on parallax. HD 95808 is a G-type giant star.

Okayama Planet Search team has published a paper in late 2008 reporting investigations on radial velocity variations observed for a set of evolved stars, announcing possible detection of a substellar companion orbiting the giant star HD 203857. Orbital period is estimated 2.3 years, but planet has still to be confirmed.

The larger member of the pair is a giant star with 1.75 times the mass and 24 times the luminosity of the Sun, while the secondary component is a subgiant star that has 1.47 times the Sun's mass and around 8 times the Sun's luminosity. The system is around 1.8 billion years old.

Aldebaran b is an exoplanet orbiting the orange giant star Aldebaran, 65 light-years away. It was initially detected in 1993, but was considered doubtful until in 2015, when researchers came to a conclusion that there is likely an exoplanet orbiting Aldebaran, consistent with the original calculations, but also compatible with stellar activity.

This is an aging giant star with a stellar classification of K1III, having exhausted is core hydrogen then cooled and expanded off the main sequence. It has 12.6 times the girth of the Sun and is radiating 67 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,643 K.

HD 50235 is a class K5III (orange giant) star located approximately 811 light years away, in the constellation Puppis. Its apparent magnitude is 4.99. HD 50235 made its closest approach to the Sun 7.8 million years ago, at the distance of 137 light years, during which it had an apparent magnitude of 1.13.

Exocomets are suggested as one source of white dwarf pollution. After a star from the main sequence becomes a giant star, it loses mass. Planetesimals in an analog of the solar Oort Cloud can be directed toward the inner stellar system. This is a consequence of the mass-loss during the AGB stage.

Xi Aquilae (ξ Aquilae, abbreviated Xi Aql, ξ Aql), officially named Libertas , is a red clump giant star located at a distance of from the Sun in the equatorial constellation of Aquila. As of 2008, an extrasolar planet (designated Xi Aquilae b, later named Fortitudo) has been confirmed in orbit around the star.

The stellar classification of this star is K3 IIIa, where the luminosity class of III indicates that this is an evolved giant star. It is around 37 times the radius of the Sun. and shines with a luminosity approximately 1279 times that of the Sun and has a surface temperature of 4320 K.

This is an evolved giant star with a stellar classification of G8III that has swollen and cooled off the main sequence. At present it has 22 times the radius of the Sun. It shines with a luminosity approximately 226 times that of the Sun and has an effective temperature of 4,787 K.

The planet orbits a (K-type) giant star named Epsilon Tauri. It has exhausted the hydrogen supply in its core and is currently fusing helium. The star has a mass of 2.7 and a radius of around 12.6 . It has a surface temperature of 4901 K and is 625 million years old.

This is an evolved K-type giant star with a stellar classification of K5 III. It has about the same mass as the Sun, but has expanded to 44.7 times the Sun's radius. The star is radiating 391 times the solar luminosity from its outer atmosphere at an effective temperature of 3,930 K.

At the age of about two billion years, this is an evolved G-type giant star with a stellar classification of G8 III-IIIb. It has 2.39 times the mass of the Sun and is radiating 69 times the Sun's luminosity from its photosphere at an effective temperature of around 4,965 K.

This star has a stellar classification of A0 III, matching that of an A-type giant star. It has a relatively high rate of spin with a projected rotational velocity of 154 km/s. The star is radiating 286 times the Sun's luminosity from its photosphere at an effective temperature of 9,980 K.

Stars #28 and #105 are Wolf-Rayet stars. Star #27, a blue giant star with a spectral type of O8III((f)), may be one of the most luminous stars known, with a bolometric magnitude of −10.5. Star #102 is known as V925 Scorpii or HD 159378, and is a rare yellow supergiant star.

Kepler-432 A is a K-type giant star. It has exhausted the hydrogen in its core and has begun expanding into a red giant. The star has a mass and radius 132% and 406% that of the Sun. It has a temperature of 4995 K and is 4.2 billion years old.

Darkover is the planet giving its name to the Darkover series of science fiction-fantasy novels and short stories by Marion Zimmer Bradley and others published since 1958.Darkover - Marion Zimmer Bradley Literary Trust According to the novels, Darkover is the only habitable planet of seven orbiting a fictional red giant star called Cottman.

Eta2 Hydri b (η2 Hyi b, η2 Hydri b), commonly known as HD 11977 b, is an extrasolar planet that is approximately 217 light-years away in the constellation of Hydrus. The presence of the planet around an intermediately massive giant star provides indirect evidence for the existence of planetary systems around A-type stars.

Rho2 Arietis is an M-type red giant star in the northern constellation of Aries. With an annual parallax shift of 9.28 mas, it is approximately distant from the Earth. Rho2 Arietis is classified as a semiregular variable star with periods of 49.9 and 54.8 days. It varies in visual magnitude between 5.45 and 6.01.

The two stars take at least 1150 years to orbit each other. The system is 85.6 ± 0.8 light-years away from the Sun. Epsilon and Zeta Crateris mark the Cup's rim. The largest naked eye star in the constellation, Epsilon Crateris is an evolved K-type giant star with a stellar classification of K5 III.

The brighter star is a giant of spectral type K2III, while the companion is a main sequence star of spectral type B9.5V. Nu Canis Majoris is a yellow-hued giant star of magnitude 5.7, 278 light-years away; it is at the threshold of naked- eye visibility. It has a companion of magnitude 8.1.

HD 88836 is a double star in the southern constellation of Antlia. With an apparent magnitude of 6.35, it is faintly visible to the naked eye from dark skies. The brighter component is a giant star with a stellar classification of G8III. It is radiating energy at a luminosity 58 times that of the Sun.

HD 220766 is a double star in the equatorial constellation of Aquarius. The primary is a K-type giant star with a stellar classification of K0III and an apparent magnitude of 6.44. It has a faint, magnitude 12 companion, located at an angular separation of 5.0″ along a position angle of 132° (as of 1933).

At 2.2 billion years old, 51 Aurigae has evolved off from the main sequence and is now a K-type giant star. It is 1.58 times as massive as the Sun, 24.5 times as wide, and 178 times as luminous. It emits radiation from its photosphere with an effective temperature of about 4,277 K.

This is an evolved giant star of stellar class K1 III. It has 12 times the radius of the Sun and shines with 60 times the Sun's luminosity. This energy is being radiated from its outer atmosphere at an effective temperature of 4,603 K, giving it the cool orange hue of a K-type star.

Abt and Morrell (1995) found a stellar classification of F0 IV for this star, suggesting it is an F-type subgiant. In their 2010 study, Fox Machado et al. assigned a class of F2 III, which matches an evolved giant star. It is a Delta Scuti variable with at least three overlapping pulsation frequencies.

HD 177809 is a 6th magnitude star in the constellation Lyra, approximately 700 light years away from Earth. It is a red giant star of the spectral type M2III, meaning it possesses a surface temperature of under 3,500 kelvins. In comparison to our Sun, it is much larger and brighter, but its surface is cooler.

It is drifting further away with a radial velocity of +21 km/s. At one time it was a candidate member of the Zeta Herculis Moving Group but has since been excluded. This object is an aging red giant star on the asymptotic giant branch with a stellar classification of M3/4III. Samus et al.

It is a candidate member of the Volans-Carina Association of co-moving stars. The visible component is an aging bright giant star with a stellar classification of B8/9II. The spectrum of the star displays metallic lines of magnesium. The Volans-Carina Association to which it belongs has an age of 90 million years.

HD 177808 is a 6th magnitude star in the constellation Lyra, approximately 610 light years away from Earth. It is a solitary red giant star of the spectral type M0III, meaning it possesses a surface temperature of around 3,940 kelvins. It is therefore much larger and brighter than our Sun, yet cooler in comparison.

This is a spectroscopic binary star system with an estimated period of 2,500 days. The primary component is a red giant star with a stellar classification of M1.5 III. The outer envelope of this evolved star has expanded to 35 times the size of the Sun. The star has the same mass as the Sun.

HD 240210 b is a 6.9 Jupiter-mass exoplanet discovered on June 10, 2009 by Niedzielski et al. using the Hobby-Eberly Telescope. It orbits the K3 giant star HD 240210 in the constellation of Cassiopeia. Its average orbital separation is at 1.33 Astronomical Units away from its star with a year of 501.75 days.

Kappa Herculis A is a giant star with stellar classification G8III. With a mass of and radius that is , the star boasts a bolometric luminosity that is . Its slightly companion is cooler and about a third of the luminosity. Kappa Herculis is a suspected variable star with a reported magnitude range of 4.70 to 5.02.

This is an evolved giant star with a stellar classification of G8.5 III. It is reported as a RS CVn variable with magnitude varying by 0.02 mag. and showing a high level of chromospheric activity. The star has 2.54 times the mass of the Sun and has expanded to 9.20 times the Sun's radius.

HD 211392 is a suspected variable star in the equatorial constellation of Aquarius, positioned about 370 light-years away. With an apparent magnitude close to six, according to the Bortle scale it is just visible to the naked eye from dark, rural skies. It is a giant star with a stellar classification of K3III.

The primary component is a magnitude 4.48 evolved giant star with a stellar classification of K4.5 III. The measured angular diameter, after correction for limb darkening, is . At the estimated distance of Omega Lupi, this yields a physical size of about 40 times the radius of the Sun. The companion is a magnitude 11.0 star.

However, between November 1 and 10, the two streams equalize. The brightest member of this constellation is Aldebaran, an orange-hued, spectral class K5 III giant star. Its name derives from ' ', Arabic for "the follower", probably from the fact that it follows the Pleiades during the nightly motion of the celestial sphere across the sky.

Kepler-432 is a binary star system composed of a K-type giant star (Kepler-432 A) and a red dwarf star (Kepler-432 B). The apparent magnitude of the system, or how bright it appears from Earth's perspective, is about 15.8. Therefore, it is too dim to be seen with the naked eye.

HD 156091 is a double star in the southern constellation of Ara. The primary is a sixth magnitude giant star with stronger than normal lines of carbon, nitrogen, and barium in its spectrum. The companion is a 13th magnitude star at an angular separation of 27.4″ along a position angle of 275°, as of 2000.

HD 102272 c is an extrasolar planet approximately 1,200 light-years away in the constellation of Leo. The planet is orbiting the K-type giant star HD 102272. The planet was discovered by the radial velocity method, using the Hobby-Eberly Telescope. Another planet, HD 102272 b, was also discovered orbiting the same star.

Omicron Virginis (ο Vir, ο Virginis) is a star in the zodiac constellation of Virgo. It is visible to the naked eye with an apparent visual magnitude of +4.12. Based upon parallax measurements, it is about 163 light years from the Sun. ο Virginis is a G-type giant star with a stellar classification of G8 IIIa CN-1Ba1CH1.

This indicates that it is a Barium star. Typically Barium stars are close binaries with a white dwarf companion, but no companion has been detected for ο Virginis. It has been suggested that an excess SiIV emission flux is due to an unseen white dwarf companion. ο Virginis is a giant star around tens times larger than the sun.

This is an evolved K-type giant star with a stellar classification of K1 III. It has 1.59 times the mass of the Sun, while its diameter has been estimated as around 11 times that of the Sun. The star is radiating 61 times the Sun's luminosity from its enlarged photosphere at an effective temperature of around 4,600 K.

Delta Pictoris (δ Pic) is a class B3III (blue giant) star in the constellation Pictor. Its apparent magnitude is 4.72 and it is approximately 1300 light years away based on parallax. It is a β Lyrae variable, a type of eclipsing binary, which ranges in brightness from 4.90 to 4.65 magnitude with a period of 1.67 days.

The star is situated near the ecliptic and thus is subject to lunar occultations. This is an aging K-type giant star with a stellar classification of K4III. Having exhausted the supply of hydrogen at its core, it has cooled and expanded off the main sequence. At present it has 41 times the girth of the Sun.

At that distance, the visual magnitude of this star is diminished by 0.15 from extinction due to interstellar dust. This is an A-type main-sequence star with a stellar classification of A0 V, per Houk (1979). However, Gray & Garrison (1987) have it classed as B9.5 III-n, suggesting it is a more evolved giant star.

The planet orbits a (K-type) giant star named Iota Draconis. The star has exhausted the hydrogen supply in its core and is currently fusing helium. The star has a mass of 1.82 and a radius of around 12 . It has a surface temperature of 4545 K and is around 800 million years old based on its evolution.

SPHERE and VLT NACO image of the nebulosity forming around L2 Puppis (Credit: ESO/P. Kervella) L2 Puppis (also known as HD 56096) is a giant star in the constellation of Puppis and is located between the bright stars Canopus and Sirius. It is a semi-regular pulsating star. The designation L2 has a tangled history.

Perkins et al. (1989) found a stellar classification of for this star, suggesting it is a K-type giant with abundance anomaly of barium. Houk and Swift (1999) matched an ordinary giant with a class of K3 III. Many sources still use the 1991 Bright Star Catalogue classification of K5 II, which instead suggests a bright giant star.

This object is an evolved giant star with a stellar classification of K4 III. As a result of having exhausted the hydrogen at its core, it has expanded to 28 times the radius of the Sun. The star is radiating 203 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,119 K.

This is a giant star with a stellar classification of K4 III. It is a suspected variable star that apparently ranges in magnitude between 4.35 and 4.45. The measured angular diameter of this star is . At the estimated distance of Delta Ophiuchi, this yields a physical size of about 33 times the radius of the Sun.

This is an evolved giant star of type K with a stellar classification of K2 III. Wittkowski et al. (2017) consider it to have a luminosity class of II-III, suggesting it is in a transitional zone between giants and supergiant stars. It has around 5 times the mass of the Sun and 73 times the Sun's radius.

This is a single-lined spectroscopic binary system with an orbital period of and an eccentricity of 0.4. The visible component is an evolved giant star with a stellar classification of K4 III. Its measured angular diameter is . At the estimated distance of the star, this yields a physical size of about 38 times the radius of the Sun.

This is an F-type giant star with a stellar classification of F3 III. The measured angular diameter is , which, at its estimated distance, yields a physical size of about 3.7 times the radius of the Sun. It radiates approximately 24 times the solar luminosity from an outer atmosphere at an effective temperature of 6,309 K.

This is a double-lined spectroscopic binary. The spectrum matches a stellar classification of B7 IV, which would indicate a subgiant star that has exhausted the supply of hydrogen at its core and is in the process of evolving into a giant star. Xi Arietis was once a designation for Psi Ceti (ψ Cet, ψ Ceti).

HD 180450 is a 6th magnitude star in the constellation Lyra, approximately 1,400 light years away from Earth. It is a red giant star of the spectral type M0III, meaning it has a surface temperature of about 3,500 kelvins. It is much larger and brighter, yet cooler, than our Sun. It is also a star in a star cluster.

LY Aurigae is a close visual binary. The two stars are magnitude 6.85 and magnitude 8.35 0.6 arc-seconds apart. Each star is also a spectroscopic binary. LY Aur A is a double-lined spectroscopic binary with an O9 bright giant and an O9 giant star in contact and eclipsing each other as they orbit every 4 days.

An illustration of the structure of the Sun and a red giant star, showing their convective zones. These are the granular zones in the outer layers of these stars. Granules—the tops or upper visible sizes of convection cells, seen on the photosphere of the Sun. These are caused by the convection in the upper photosphere of the Sun.

HD 91496 (HR 4142) is a giant star in the constellation Carina, with an apparent magnitude is 4.92 and an MK spectral class of K4/5 III. It has been suspected of varying in brightness, but this has not been confirmed. HD 91496 has a faint companion, six magnitudes fainter and away. It is a distant background star.

The planet orbits a (K-type) giant star named HD 240237. It has exhausted the hydrogen supply in its core and is currently fusing helium. The star has a mass of 1.69 and a radius of around 32 . It has a surface temperature of 4361K and is likely 2 billion years old based on its mass and evolution.

Xi Aquilae b (abbreviated ξ Aquilae b, ξ Aql b), formally named Fortitudo , is an extrasolar planet approximately 200 light-years from the Sun in the constellation of Aquila. The planet was discovered orbiting the yellow giant star Xi Aquilae in 2008. The planet has a minimum mass of 2.8 Jupiter and a period of 137 days.

However, Tokovinin (2008) considers it a triple star system. Orbital elements for the main spectroscopic binary, components Aa and Ab, were published by Mayer et al. (2014), giving an orbital period of 12.76 days and an eccentricity of 0.18. This system displays a merged stellar classification of O9.5 III, matching a blue-hued O-type giant star.

The combined stellar classification is K5 III, which matches the spectrum of a giant star. The measured angular diameter of the primary star is . At the estimated distance of this system, this yields a physical size of about 107 times the radius of the Sun. The primary component shows the behavior of a slow irregular variable.

1 Lupi is a solitary giant star in the southern constellation of Lupus. It has the Bayer designation i Lupi; 1 Lupi is the Flamsteed designation. The apparent visual magnitude is 4.90, which indicates it is faintly visible to the naked eye. Based on parallax measurements, this star is approximately 1,800 light years from the Sun.

RT TrA is a cool giant star with a radius of , although its spectral luminosity class verges on the supergiant level at times during its pulsations. As it pulsates, the effective temperature varies between 5,200 and 6,500 K and its luminosity between . Its physical properties place it on the instability strip of the H–R diagram.

The visible component is an aging giant star with a stellar classification of K0III; a star that has used up its core hydrogen and is cooling and expanding. It now has 15 times the girth of the Sun and is radiating 98.5 times the Sun's luminosity from its swollen photosphere at an effective temperature of 4,737 K.

24 Cancri (abbreviated to 24 Cnc) is a triple star system in the constellation Cancer. The system is located about 260 light-years (80 parsecs) away, based on its parallax. The system has a combined apparent magnitude of 6.91. The primary component in the star system is designated 24 Cancri A. It is a F-type giant star.

It lies near the same line of sight as the sub-giant star HD 101212, although it is unclear whether these two stars are gravitationally bound or even in physical proximity. The space velocity components of this star are = . It is orbiting the galaxy at a mean distance of from the core with an eccentricity of 0.06.

This is an old, evolved K-type giant star with a stellar classification of K4 III. It is about ten billion years old with 0.95 times the mass of the Sun, but has expanded to 32 times the Sun's radius. The star is radiating 263 times the Sun's luminosity from its photosphere at an effective temperature of 4,145 K.

Iota Eridani (ι Eri) is a solitary star in the constellation Eridanus. It is visible to the naked eye with an apparent magnitude of 4.11. With an annual parallax shift of 0.02165 arcseconds, it lies at an estimated distance of about 151 light years. This is an evolved red clump giant star with a stellar classification of K0 III.

In the process it will overflow its Roche lobe and begin to transfer mass onto the secondary. This may cause the secondary to acquire enough mass to become the primary component. After both stars have passed through the giant star stage, the end result will be a pair of co-orbiting white dwarfs in about eight billion years.

Gamma Capricorni (γ Capricorni, abbreviated Gamma Cap, γ Cap), named Nashira , is a giant star in the constellation of Capricornus. Based on parallax measurements obtained during the Hipparcos mission, it is about 139 light- years from the Sun. It is 2.56 degrees south of the ecliptic, so it can be occulted by the Moon, and (rarely) by planets.

A comparison of the star Aldebaran to the size of the Sun Aldebaran (Alpha Tauri) is a type K5 giant star in the constellation Taurus that is frequently featured in works of science fiction. Aldebaran is a subject for ancient myths in multiple cultures (Inuit, Mexican, Native American) and, in more recent times, the mythologizing of science fiction.

HD 102272 b is an extrasolar planet approximately 1,200 light-years away in the constellation of Leo. The planet was discovered orbiting the K-type giant star HD 102272 in 2008. The planet was discovered by the radial velocity method, using the Hobby-Eberly Telescope. Another planet, HD 102272 c, was also discovered orbiting the same star.

This object is an aging K-type giant star with a stellar classification of K3/4III. Having exhausted the supply of hydrogen at its core, it has cooled and expanded; now having 31 times the radius of the Sun. It is radiating 274 times the Sun's luminosity from its swollen photosphere at an effective temperature of 4,189 K.

Psi4 Aurigae, Latinized from ψ4 Aurigae, is a single, orange-hued star in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of +5.02. With an annual parallax shift of , it is approximately distant from Earth. This is a K-type giant star with a stellar classification of K5 III.

Toward a Better Understanding of the Distance Scale from RR Lyrae Variable Stars: A Case Study for the Inner Halo Globular Cluster NGC 6723, ApJS, 210, 1 Consequently, the computed distance is wrong, and more importantly, certain researchers have argued that the blending effect can introduce a systematic uncertainty into the cosmic distance ladder, and may bias the estimated age of the Universe and the Hubble constant. M3. Note the characteristic "knee" in the curve at magnitude 19 where stars begin entering the giant stage of their evolutionary path. The most massive main- sequence stars will also have the highest absolute magnitude, and these will be the first to evolve into the giant star stage. As the cluster ages, stars of successively lower masses will also enter the giant star stage.

The non-classical kinds of carbon stars, belonging to the types C-J and C-H, are believed to be binary stars, where one star is observed to be a giant star (or occasionally a red dwarf) and the other a white dwarf. The star presently observed to be a giant star accreted carbon-rich material when it was still a main-sequence star from its companion (that is, the star that is now the white dwarf) when the latter was still a classical carbon star. That phase of stellar evolution is relatively brief, and most such stars ultimately end up as white dwarfs. These systems are now being observed a comparatively long time after the mass transfer event, so the extra carbon observed in the present red giant was not produced within that star.

With an apparent visual magnitude of +3.3, this is one of the brighter members of the constellation. The distance of this star from Earth is roughly , based upon parallax measurements. This is a spectral type K1 giant star with about . The stellar envelope is slightly cooler than the Sun with an effective temperature of 4,459 K, giving the star a light orange color.

Sigma Virginis (σ Vir, σ Virginis) is a star in the zodiac constellation of Virgo. It can be faintly seen with the naked eye with a baseline apparent visual magnitude of 4.86. Based upon parallax measurements, the distance to this star is roughly 680 light years. This is an evolved red giant star with a stellar classification of M1 III.

The system is about 360 million years old. The primary component is a giant star with an apparent magnitude of 2.7 and a stellar classification of G5 III. It is radiating about 107 times the luminosity of the Sun from an expanded atmosphere about 13 times the Sun's radius. The mass of this star is 3.3 times that of the Sun.

This is an aging K-type giant star with a stellar classification of K4 III, which indicates it has exhausted the hydrogen at its core and evolved away from the main sequence. The star has expanded to 30 times the radius of the Sun and is radiating 341 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,257 K.

The variable velocity of this system was reported by W. W. Campbell in 1918. It is a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.4. The components have a visual magnitude difference of 2.7 and are unresolved by speckle interferometry. The primary component is an evolved bright giant star with a stellar classification of G5II.

HD 155233 b is a confirmed exoplanet orbiting around the K Giant star HD 155233 every 885 days some 244.94 light-years away. It has a mass of 636 Earth masses or 2 Jupiter masses and is likely a gas giant similar of that to Jupiter just double the mass. It was discovered by Wittenmyer et al. on October 22nd 2015.

It is visible to the naked eye with a slightly variable apparent magnitude of about 4.5. The primary component, ο Cassiopeiae A, is a spectroscopic binary, and its close companion completes one orbit every 2.83 years (1,031.55 days). The system has also been resolved with interferometry. The primary of this spectroscopic binary is a blue-white B-type giant star.

Kappa Aurigae, Latinized as κ Aurigae, is the Bayer designation for a star in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of 4.3. Based upon an annual parallax shift of 19.31 mas, it is approximately distant from Earth. This is an evolved giant star with a stellar classification of G8.5 IIIb.

It is moving further away with a heliocentric radial velocity of 18 km/s. A preliminary orbit for the pair gives a period of and an eccentricity of 0.4. The primary component is an aging giant star with a stellar classification of K4/5 III. It is radiating 495 times the Sun's luminosity from its photosphere at an effective temperature of 3,951 K.

At that distance, the star's brightness is reduced by 0.33 in magnitude because of extinction from interstellar gas and dust. This is a red giant star with a stellar classification of M3 III. The measured angular diameter of this star is . At the estimated distance of Delta Ophiuchi, this yields a physical size of about 67 times the radius of the Sun.

The distance to this system, based upon an annual parallax shift of , is around 660 light years. It is moving closer to the Earth with a heliocentric radial velocity of −32 km/s. The primary component is an aging giant star with a stellar classification of K4 III. It is a suspected variable star of unknown type with a maximum magnitude of 5.48.

It is moving closer to the Earth with a heliocentric radial velocity of −13 km/s. This is an aging K-type giant star with a stellar classification of . It shows a spectral anomaly with the absorption lines of cyanogen (CN). This is a red clump giant, indicating that it is generating energy through the helium fusion at its core.

The two components of this system have an angular separation of 0.25 arcseconds. The brighter component is a giant star with a spectral classification of G8 III and an apparent magnitude of 4.79. The effective temperature of its outer atmosphere is 4,900 K, giving it the yellowish glow of a G-type star. The fainter component is a star of magnitude 6.77.

This is an aging giant star with a stellar classification of G8 III. It is most likely on the horizontal branch and is a candidate red clump giant. The star is an estimated 1.46 billion years old with 2.15 times the mass of the Sun. With the hydrogen at its core exhausted, it has expanded to 12 times the Sun's radius.

This is an evolved giant star with a stellar classification of G7 IIIa. It is a suspected variable star of unknown type, and is an X-ray source. The star is 370 million years old with 3.27 times the mass of the Sun. Having exhausted the hydrogen at its core, the star has expanded to 23 times the Sun's radius.

This is an aging giant star with a stellar classification of K1III, having exhausted the supply of hydrogen at its core and expanded to 19 times the Sun's radius. It is four billion years old with 1.11 times the mass of the Sun. The star is radiating 132 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,458 K.

This is an evolved bright giant star with a stellar classification K2II, between the classifications of giant and supergiant. Having exhausted the supply of hydrogen at its core, it has expanded to around 33.5 times the radius of the Sun. The star is radiating 469 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,642 K.

HD 4732 is a red giant star of magnitude 5.9 located in the constellation Cetus. It is 189 light years from the solar system. HD 4732 is located in the celestial Southern Hemisphere, although it can be observed from most regions of the Earth. Near Antarctica the star is circumpolar, while it is always below the horizon near the Arctic.

According to the R.H. Allen's works, it shares names with ζ Aquilae.Star Names - R.H.Allen p.61 Epsilon Aquilae is more precisely called Deneb el Okab Borealis, because is situated to the north of Zeta Aquilae, which can therefore be called Deneb el Okab Australis. The primary component of this system is an evolved giant star with a stellar classification of K1 III.

Q Scorpii (Q Sco) is an orange giant star in the constellation Scorpius. Its apparent magnitude is 4.27. It lies in the tail of Scorpius, between the stars λ Scorpii and μ Scorpii, from the faint globular cluster Tonantzintla 2. Q Scorii is a suspected astrometric binary, a star whose position is seen to oscillate although no companion has been detected.

Judging from its motion through space, it is a candidate member of the Sirius supercluster. This object is a superficially normal A-type star. However, there is some disagreement over the evolutionary state of the star, as it has received luminosity classifications of a subgiant, main sequence, and a giant star. Unexpectedly for an A-type star, a magnetic field has been detected.

Xi Leonis (ξ Leo, ξ Leonis) is a solitary star in the zodiac constellation of Leo. It has an apparent visual magnitude of 5.1 and is faintly visible to the naked eye. The distance to this star, as determined by parallax measurements, is roughly 216 light years. This is an evolved, K-type giant star with a stellar classification of K0 III.

Tau2 Aquarii (τ2 Aqr, τ2 Aquarii) is the Bayer designation for a star in the equatorial constellation of Aquarius. It is visible to the naked eye with an apparent visual magnitude of +4.0. Because the star lies near the ecliptic it is subject to occultations by the Moon. This is an orange-hued giant star with a stellar classification of K5 III.

The spectrum of 88 Aquarii matches an evolved giant star with a classification of K1 III. Its measured angular diameter is , which, at the estimated distance of Delta Ophiuchi, yields a physical size of about 29 times the radius of the Sun. The cool, orange hued glow of this star comes from the outer atmosphere's effective temperature of 4,430 K.

Chi Aquarii, Latinized from χ Aquarii, is the Bayer designation of a star in the equatorial constellation of Aquarius. The distance to this star, based upon parallax measurements with a 7% margin of error, is roughly . It is visible to the naked eye with an apparent visual magnitude of +5.06. This is a red giant star with a spectral classification of M3 III.

This is an evolved K-type giant star with a stellar classification of K4 III, having used up its core hydrogen and has expanded to around 45 times the radius of the Sun. It is a suspected variable star, with a brightness that varies about 0.03 in magnitude. The relatively cool outer atmosphere has an effective temperature of 3999 K.

This is an evolved red giant star with a stellar classification of K5 III. The measured angular diameter of Nu2 Coronae Borealis is . At its estimated distance, this yields a physical size of about 50 times the radius of the Sun. Nu2 Coronae Borealis is radiating 530 times the Sun's luminosity from its photosphere at an effective temperature of 3,940 K.

The system is a source of X-ray emission. The visible component is an aging giant star with a stellar classification of G8 III. At the age of 1.15 billion years, it has exhausted the hydrogen at its core region and expanded off the main sequence. It is about 13 times the Sun's radius and 2.35 times the Sun's mass.

This is an aging, metal-poor giant star with a stellar classification of K1 III. It is about 9.3 billion years old with 94% of the mass of the Sun. Having exhausted the supply of hydrogen at its core, the star cooled and expanded to 23 times the Sun's radius. The star is spinning slowly, taking to complete its sidereal rotation.

Omicron Cephei, Latinized from ο Cephei, is a binary star in the constellation of Cepheus. It consists of a less massive F-type main sequence star in orbit with a more massive G-type giant star. The overall apparent visual magnitude of the system is 4.75. The pair was first determined to be binary by F. G. W. Struve in 1832.

The system is moving away from the Sun with a radial velocity of +30 km/s. Epsilon Cancri A is a double-lined spectroscopic binary system with an orbital period of 35 days and eccentricity of 0.32. It has a stellar classification of A5 III, which matches an A-type giant star. The spectrum displays the chemically peculiar characteristics of an Am star.

Keenan and McNeil (1989) classified it as , indicating it is a giant star showing a deficiency of iron and an excess of cyanogen in its atmosphere. However, Gray et al. (2006) listed it as , which would suggest a less evolved subgiant star. It may be a red clump star, which indicates it is generating energy through helium fusion at its core.

Iota Cephei (ι Cephei, ι Cep) is a star in the northern constellation Cepheus. Based upon an annual parallax shift of as seen from the Earth, it is located about from the Sun. The star is visible to the naked eye with an apparent visual magnitude of 3.5. It is a K-type giant star with a stellar classification of K0 III.

The primary is a silvery giant of magnitude 4.9, and the secondary is an old, reddish giant star of magnitude 5.2. The star HD164669 near the primary may be an optical double. 100 Herculis is a double star easily divisible in small amateur telescopes. Both components are magnitude 5.8 blue-white stars; they are 165 and 230 light-years from Earth.

A is an A-type giant star, while B is a B-type subgiant star. They are also referred to, rarely, as Rho1 Herculis and Rho2 Herculis. Rho Herculis A is itself a close binary which has been resolved using speckle interferometry, with the two components separated by . The two visual components have very similar spectral types, between A0 and B9.

Some studies suggest that this star is a luminous AGB star and a long-period variable, instead of a supergiant. It is classified in the General Catalogue of Variable Stars as a semiregular variable star of type SRb, indicating a cool pulsating giant star, with a possible period of 655 days. Its brightness varies between extremes of magnitude 7.7 and 9.2.

This is an evolved G-type giant star with a stellar classification of G8 III. It is classified as a BY Draconis type variable star. This is a chromospherically- active star with a longitudinal magnetic field strength of and an X-ray luminosity of . The activity and photometric variation of the star allow an estimate of its rotation period as 68 days.

HD 122430 is single star in the equatorial constellation of Hydra. It has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude of 5.47. The star is located at a distance of 105.6 light years from the Sun based on parallax. This is an aging giant star with a stellar classification of K2–3III.

Beta Tauri (Latinised from β Tauri, abbreviated Beta Tau, β Tau), officially named Elnath (pronounced or , sometimes spelled Alnath), is the second- brightest star located in the constellation borders of Taurus and Auriga with an apparent magnitude of 1.65. It is a chemically peculiar B7 giant star, 134 light years away from Earth. It had a co-existing name Gamma Aurigae.

It is moving closer with a heliocentric radial velocity of −11 km/s. This is a solitary, G-type giant star with a stellar classification of G8 III. It is around 270 million years old with 3.6 times the mass of the Sun. Having exhausted the supply of hydrogen at its core, it has expanded to 26 times the Sun's radius.

This is an aging giant star with a stellar classification of K3 III that is most likely (86% chance) on the horizontal branch. The star has 2.9 times the mass of the Sun and has expanded to 40 times the Sun's radius. It is radiating 569 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,300 K.

At the age of about 234 million years, is an evolved, G-type giant star with a stellar classification of G8 III. It has an estimated 3.6 times the mass of the Sun and has expanded to 24 times the Sun's radius. It is radiating 310 times the Sun's luminosity from its photosphere at an effective temperature of 4,994 K.

31 Comae Berenices (31 Com) is a yellow giant star in the constellation Coma Berenices. Its apparent magnitude is about 4.9 and slightly variable. It is a rare FK Comae Berenices variable, a variable star that spins rapidly and has large starspots on its surface. It is currently in the Hertzsprung gap and its outer envelope has just begun convection.

There is disagreement in the literature as to the stellar classification of this star. Malaroda (1975) has it catalogued as F1 III, which would suggest it is an evolved F-type giant star. Houk (1979) listed it as F3 IV/V, which appears to indicate a less evolved F-type star transitioning between the main sequence and subgiant star. Gray et al.

Observational studies of their radial velocity suggested that all barium stars are binary stars. Observations in the ultraviolet using International Ultraviolet Explorer detected white dwarfs in some barium star systems. Barium stars are believed to be the result of mass transfer in a binary star system. The mass transfer occurred when the now-observed giant star was on the main sequence.

Zeta Caeli, Latinized from ζ Caeli, is an orange-hued star in the constellation Caelum with a visual magnitude of +6.36. It is an evolved K-type giant star and a member of the Milky Way's thick disk population. Based upon an annual parallax shift of 7.59 mas as seen from Earth, this star is located about 430 light years from the Sun.

Psi9 Aurigae, Latinized from ψ9 Aurigae, is a star in the northern constellation of Auriga. It is dimly visible to the naked eye with an apparent visual magnitude of 5.75. Based upon an annual parallax shift of 2.59 mas, the distance to this star is approximately . The spectrum of Psi9 Aurigae matches a giant star with a stellar classification of B8 IIIe.

The primary component is an evolved red giant star with a stellar classification of M3 IIICa-1. It is an irregular variable with seven measured pulsation periods ranging from 22.4 to 162.6 days, and amplitudes ranging up to 0.m022. The star is a bright X-ray source with a luminosity of . There is a magnitude 8.3 companion at an angular separation of 0.04 arcseconds.

Adhafera is a giant star with a stellar classification of F0 III. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified. Its apparent magnitude is +3.44, making it relatively faint for a star that is visible to the naked eye. Nevertheless, it shines with 85 times the luminosity of the Sun.

Based upon an annual parallax shift of 27.10 mass, Iota Geminorum lies some 120.4 light years from the Sun. This is an evolved red clump giant star with a stellar classification of G9 III. It is most likely a member of the galactic thin disk population. The star has 1.89 times the mass of the Sun, but has expanded to 10 times the solar radius.

This is a probable astrometric binary system with the components having an angular separation of 7.2 arcseconds along a position angle of 241°, as of 2014. The primary is an evolved G-type giant star with a stellar classification of G9 III. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.

This is an evolved F-type giant star with a stellar classification of F2 III that has swollen and cooled off the main sequence after consuming the hydrogen at its core. It is an estimated 1.5 billion years old with 1.74 times the mass of the Sun. Zeta Normae is radiating approximately 16 times the Sun's luminosity from its photosphere at an effective temperature of 6,691 K.

The inner pair form a single-lined spectroscopic binary with an orbital period of 2.29 days following a circular orbit with an eccentricity of 0.00. The primary, component Aa, has a visual magnitude of 3.54. It is a white-hued G-type giant star with a stellar classification of . This indicates it is a chemically peculiar Ap star with an abnormal abundance of strontium.

This object is an aging red giant star with a stellar classification of M0.5III. After exhausting the supply of hydrogen at its core, the star cooled and expanded off the main sequence, and now has around 51 times the Sun's radius. It is radiating 628 times the luminosity of the Sun from its photosphere at an effective temperature of 4,033 K. This is a suspected variable star.

Omega1 Tauri is a solitary, orange hued star in the zodiac constellation of Taurus. It is faintly visible to the naked eye with an apparent visual magnitude of +5.51. Based upon an annual parallax shift of 11.22 mas as seen from Earth, it is located about 290 light years from the Sun. This is an evolved K-type giant star with a stellar classification of K2 III.

This is an evolved K-type giant star with a stellar classification of K0.5 IIIa. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of this star, this yields a physical size of about 10.5 times the radius of the Sun. It has an estimated 1.76 times the mass of the Sun and is about 1.7 billion years old.

It is moving closer to the Earth with a heliocentric radial velocity of −25 km/s. This body has a stellar classification of B9 III, matching a late B-type giant star. It is a chemically peculiar star of a weak Mercury-Manganese type (CP3), and is the most chromium–deficient star known. The star may possess a magnetic field with a strength greater than .

AG Draconis spends most of its time in a quiescent phase near visual magnitude 9.8, with only small semi-regular variations thought to be due to pulsations of the giant star. At its faintest, it can reach magnitude 10.3. The semi-regular variations have periods of 340 - 370 days. Variations at ultraviolet wavelengths occur with a period of 550 days, which is the orbital period.

Epsilon Columbae, Latinized from ε Columbae, is a star in the southern constellation of Columba. It is visible to the naked eye, having an apparent visual magnitude of 3.87. Based upon an annual parallax shift of 12.39, it is located roughly 263 light years from the Sun. This is an orange-hued K-type giant star with a stellar classification of K1 II/III.

Columba is rather inconspicuous, the brightest star, Alpha Columbae, being only of magnitude 2.7. This, a blue- white star, has a pre-Bayer, traditional, Arabic name Phact (meaning ring dove) and is 268 light-years from Earth. The only other named star is Beta Columbae, which has the alike-status name Wazn. It is an orange-hued giant star of magnitude 3.1, 87 light-years away.

Pi Chamaeleontis (π Cha) is a star located in the constellation Chamaeleon. Its apparent magnitude is 5.64. Parallax measurements by Hipparcos put the system at 135 light-years (41.5 parsecs) away. Pi Chamaeleontis is an A-type subgiant or F-type giant star with an effective temperature of about 6,900 K. It has an absolute magnitude of 2.56, a mass of , and a radius of .

The star is moving through the Galaxy at a speed of 50.6 km/s relative to the Sun. Its projected Galactic orbit carries it between 18,600 and 26,300 light-years from the center of the Galaxy. This object is an aging giant star with a stellar classification of F8III. It is currently in the Hertzsprung gap and is a source of X-ray emission.

PU Puppis (PU Pup) is a class B8III (blue giant) star in the constellation Puppis. Its apparent magnitude is 4.69 and it is approximately 620 light years away based on parallax. It is a β Lyrae variable, ranging from 4.75 to 4.69 magnitude with a period of 2.58 days. The secondary is estimated at about 5.6 magnitude, although recent observations have failed to confirm it.

Altarf represents a part of Cancer's body. At magnitude 3.9 is Delta Cancri, also known as Asellus Australis. Located 131±1 light-years from Earth, it is an orange-hued giant star that has swollen and cooled off the main sequence to become an orange giant with a radius 11 times and luminosity 53 times that of the Sun. Its common name means "southern donkey".

The primary is an evolved K-type giant star with a stellar classification of , showing an overabundance of CN in its spectrum. The star has expanded to 16 times the radius of the Sun and is radiating 120 times the Sun's luminosity from its swollen photosphere at an effective temperature of 4,743 K. The companion has a mass of at least 59% that of the Sun.

HD 106112, also known as CO Camelopardalis, is a star in the constellation Camelopardalis. It has an apparent magnitude of about 5.1, meaning that it is just barely visible to the naked eye. Based upon parallax measurements made by the Hipparcos spacecraft, this star is around 177 light years away from the Sun. HD 106112's spectral type shows that it is an A-type giant star.

The primary Ceti A is a G6III or G8III clump-giant star. The spectroscopic binary companion star is an A2V dwarf of about 2 solar masses and 30 luminosity. It is separated at 0.012 arcsec so in an orbit of 4.2 AU, smaller than the distance between Jupiter and the Sun. Xi1 Ceti A exhibits characteristics similar to an eclipsing binary, with a small white dwarf companion.

9 Equulei is an M-type star in the constellation Equuleus. It is an asymptotic giant branch (AGB) star, a star that has exhausted its core helium and is now fusing both hydrogen and helium in shells outside the core. It is also a suspected variable star with an amplitude of about 0.05 magnitudes. The spectral type is M2IIIa, meaning it is a relatively cool giant star.

11 Ursae Minoris b is an extrasolar planet which orbits the K-type giant star 11 Ursae Minoris, located approximately 390 light years away in the constellation Ursa Minor. This planet has a minimum mass of . Since inclination is not known, the actual mass is unknown. This planet may actually be a brown dwarf if a true mass is over 13 times that of Jupiter.

It is a yellow-hued giant star of magnitude 3.1, 340 light- years from Earth. The secondary is a blue-white hued star of magnitude 6.1. The two stars are distinguishable in binoculars. β Capricorni's traditional name comes from the Arabic phrase for "the lucky stars of the slaughterer," a reference to ritual sacrifices performed by ancient Arabs at the heliacal rising of Capricornus.

This is an evolved giant star with a stellar classification of K1 III. The measured angular diameter of this star, after correcting for limb darkening, is . At the estimated distance of this star, this yields a physical size of 11.6 times the radius of the Sun. It is radiating 54 times the Sun's luminosity from its enlarged photosphere at en effective temperature of 4,812 K.

Now capable of being disambiguated as Aa (from A before), the main, inner stellar component is a B3 III blue giant star. It has a mass of approximately . It and its unseen companion form an inner binary with a period of 40.33 days. The spectral type of component Aa is well-defined at about B3 from the distinct narrow lines in the composite spectrum.

It will make its closest approach in about 0.9 million years, coming within . The pair orbit each other with an estimated period of 1,201 years and an orbital eccentricity of 0.932. The magnitude 5.93 primary, component A, displays a stellar classification of F2III, matching an aging F-type giant star. This star is spinning rapidly with a projected rotational velocity of 136 km/s.

Gamma Apodis (γ Aps, γ Apodis) is the Bayer designation for a star in the southern circumpolar constellation of Apus. From parallax measurements, the distance to this star can be estimated as . It is visible to the naked eye with an apparent visual magnitude of 3.86. A stellar classification of G9 III identifies it as a giant star in the later stages of its evolution.

Tau Aurigae, Latinized from τ Aurigae, is a star in the northern constellation Auriga. It is visible to the naked eye with an apparent visual magnitude of 4.505, and is approximately distant from Earth. Tau Aurigae is an evolved giant star with a stellar classification of G8 III. It has expanded to 11 times the radius of the Sun and shines with 63 times the Sun's luminosity.

The radiant point for this shower passes several degrees to the south of the star. Delta Aurigae is a spectroscopic binary: periodic Doppler shifts in the star's spectrum indicate orbital motion. The visible component of this system is a giant star with a stellar classification of K0 III. It has 11 times the radius of the Sun and shines with 62 times the Sun's luminosity.

This is listed as an eclipsing binary system with a period of 47.9 days and has the variable star designation RR Arietis. During each eclipse of the primary star, the magnitude of the system decreases by 0.40. The eclipse of the secondary reduces the magnitude by 0.35. The primary component of the system is an evolved giant star with a stellar classification of K1 III.

The spectrum of 38 Aquarii matches a stellar classification of B5 III. A luminosity class of III indicates that this is an evolved giant star. It has 5.6 times the radius of the Sun and is spinning with a projected rotational velocity of 20 km/s. The outer atmosphere of the star has a blue-white glow from an effective temperature of 13,860 K.

This pair is positioned near the line of sight to the open cluster NGC 752, located away. The brighter primary is an aging giant star with a stellar classification of K0 III, having exhausted the hydrogen at its core and evolved off the main sequence. It is a red clump giant, having undergone "helium flash" and is presently generating energy at its core through helium fusion.

R Horologii is a red giant star approximately 1,000 light-years away in the southern constellation of Horologium. It is a Mira variable with a period of 404.83 days, ranging from apparent magnitude 4.7 to 14.3—one of the largest ranges in brightness known of stars in the night sky visible to the unaided eye. The star is losing mass at the rate of .

This is an evolved K-type giant star with a stellar classification of K5.5 III. Astroseismology was used to obtain a mass estimate of 1.11 times the mass of the Sun, while interferometric measurements give a size of about 38 times the Sun's radius. It is radiating about 332 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,920 K.

The primary, component A, has a stellar classification of B8 IIIp, suggesting it is a B-type giant star. It a mercury-manganese star, a type of chemically peculiar star showing large overabundances of those two elements in the outer atmosphere. It is classified as an Alpha2 Canum Venaticorum type variable star and its brightness varies from magnitude +5.22 to +5.27 with a period of 5 days.

The primary, component A, is a white-hued A-type giant star with a stellar classification of A0 III. It is a magnetic Ap star with a field strength of , showing abundance peculiarities in strontium, chromium, and mercury. The star has 2.8 times the mass of the Sun and is radiating 93 times the Sun's luminosity from its photosphere at an effective temperature of 10,250 K.

It has a Trumpler class of . The cluster is 33 million years old with an estimated mass of . It has one definite Be star and 29 B-type stars in total. There are three supergiant stars, all of class A or earlier. The brightest component (lucida), designated HD 168352, is a B-type giant star with a class of B2 III and a visual magnitude of 8.65.

The nebula IC 2944 lies nearby. Lambda Centauri is a B-type giant star with a stellar classification of B9 III. (Although it has also been classified as A1 III.) It has about 5.5 times the radius of the Sun and is rotating rapidly with a projected rotational velocity of . The star's outer atmosphere has an effective temperature of 9,880 K, giving it a blue-white hue.

This object is an aging giant star with a stellar classification of K3III, indicating the star has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. At present it has 39 times the girth of the Sun. It is radiating 480 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,325 K.

7 Cancri (7 Cnc) is a giant star in the constellation Cancer. Its apparent magnitude is 6.84 and it is about away. The annual parallax of 7 Cancri determined from the Hipparcos satellite mission is , giving a distance of with an 11.5% margin of error. The more recent and more accurate Gaia Data Release 2 contains a parallax of , resulting in a closer distance of .

Based on the Gaia distance, 7 Cancri has a bolometric luminosity 65 times that of the sun. Its temperature, based on its colour, is calculated to be and the resulting radius is . 7 Cancri is a cool giant star. It has evolved away from the main sequence after exhausting its core hydrogen and expanded so that it is larger and more luminous than the sun, although cooler.

78 Cancri is a star in the zodiac constellation of Cancer, located 548 light years from the Sun. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 7.19. The star is moving away from the Earth with a relatively large radial velocity of +77.7 km/s. It is an evolved giant star with a stellar classification of K3 III.

There has also been reported an observation of a bright, rapidly rotating giant star in a binary system with an unseen companion emitting no light, including x-rays, but having a mass of solar masses. This is interpreted to suggest that there may be many such low-mass black holes that are not currently consuming any material and are hence undetectable via the usual x-ray signature.

After around fifty hours while the game has been running, the mountain meets its fate when it crashes into a passing giant star, ending the game, at which point the player can start the game over with a new mountain. This can be avoided by repeatedly pressing buttons on one's keyboard which forms a shield around the mountain that protects it from getting destroyed.

The primary component of this system is an aging giant star with a stellar classification of K3III. The star's chromosphere is of the type called "hybrid", displaying a cool stellar wind in combination with hot emission lines. It appears to be the source for the X-ray emission coming from this system. The star is 32 million years old with 8.5 times the mass of the Sun.

Mu Aquilae (μ Aql, μ Aquilae) is the Bayer designation for a star in the equatorial constellation of Aquila. With an apparent visual magnitude of 4.45, it is visible to the naked eye. The measured annual parallax shift of 30.31 mas, which is equivalent to a distance of from Earth. The stellar classification of Mu Aquilae is K3 III, indicating that this is an evolved giant star.

V337 Carinae (V337 Car, q Carinae) is a K-type bright giant star in the constellation of Carina. It is an irregular variable and has an apparent visual magnitude which varies between 3.36 and 3.44. V337 has a spectral class of K2.5II, indicating a bright giant. It is considered likely to be on the red giant branch of stars fusing hydrogen around an inert helium core.

This is a massive B-type lower-luminosity supergiant or bright giant star with a stellar classification of B1 Ib or B0.5 II, respectively. It is around 22.5 million years old with a high rate of spin, showing a projected rotational velocity of 140 km/s. J. D. Rosendhal (1973) identified weak emission features associated with an asymmetric H-alpha absorption line, providing evidence of mass loss.

This is an evolved red giant star with a stellar classification of M4.5 IIIa. It is a pulsating variable with multiple periods, including 20.6, 24.1, 24.5, and 32.3 days. The strongest period is 33.3 days with an amplitude of 0.043 magnitude. It has a magnitude 9.71 visual companion at an angular separation of 60.4 arc seconds along a position angle of 210°, as of 2013.

A giant star is a star with substantially larger radius and luminosity than a main-sequence (or dwarf) star of the same surface temperature.Giant star, entry in Astronomy Encyclopedia, ed. Patrick Moore, New York: Oxford University Press, 2002. . They lie above the main sequence (luminosity class V in the Yerkes spectral classification) on the Hertzsprung–Russell diagram and correspond to luminosity classes II and III.

Lambda Aquarii is a red giant star with a stellar classification of M2.5 III. It is classified as slow irregular variable and pulsation periods of 24.5, 32.0, and 49.5 days have been identified. This star is on the asymptotic giant branch and is generating energy through the nuclear fusion of hydrogen and helium along concentric shells surrounding an inert core of carbon and oxygen.

This is a probable astrometric binary system. The primary, component A, is an evolved giant star with a stellar classification of K0 III. It is a red clump star that is generating energy through the fusion of helium at its core. The measured angular diameter is , which, at the estimated distance of Psi Hydrae, yields a physical size of about 10.6 times the radius of the Sun.

"Giant Star" release debut album "Year Of The Snake" in 2013. He is also scheduled to appear at FC United of Manchester's much lauded 'club night in the afternoon' Course You Can Malcom on Saturday 25 January 2014, where he will be performing an acoustic Space Monkeys set. He currently tours as "Space Monkeys" with a new line up. Chas Morrison is the only other original member.

91 Aquarii is an orange giant star orbited by one planet, 91 Aquarii b. The planet's mass is 2.9 times the mass of Jupiter, and its orbital period is 182 days. Gliese 849 is a red dwarf star orbited by the first known long-period Jupiter-like planet, Gliese 849 b. The planet's mass is 0.99 times that of Jupiter and its orbital period is 1,852 days.

The Walt Disney Company India Private Limited, known simply as Disney India, is an Indian subsidiary of the Asia Pacific region of the American media and entertainment conglomerate The Walt Disney Company and headquartered in Mumbai, Maharashtra. In March 2019, post the acquisition of majority of assets of 21st Century Fox which included Indian TV giant Star India, Disney India became world's biggest television broadcaster.

A geodesic fold occurs when a Verteron beam is fired at the atmosphere of a giant star at two different locations. This connects both points in space and creates a short lived passage. However, this was not usable because of deadly radiation that occurred during flight. A Ferengi ship's faked message from the Alpha Quadrant made the crew believe there was a safe passage.

The five brightest stars are all reddish in hue. Shading the others at apparent magnitude 3.8 is Alpha Apodis, an orange giant that has around 48 times the diameter and 928 times the luminosity of the Sun. Marginally fainter is Gamma Apodis, another ageing giant star. Delta Apodis is a double star, the two components of which are 103 arcseconds apart and visible with the naked eye.

Octans is a very faint constellation; its brightest member is Nu Octantis, a spectral class K1 III giant star with an apparent magnitude 3.73. It is 63.3 ± 0.8 light-years distant from Earth. Beta Octantis is the second brightest star in the constellation. Sigma Octantis, the southern pole star, is a magnitude 5.4 star just over 1 degree away from the true South Celestial Pole.

This is an evolved giant star with a stellar classification of G7 III, most likely (93% chance) on the horizontal branch. At the age of 191 million years, it has 3.84 times the mass of the Sun but has expanded to 24 times the Sun's radius. The star is radiating 316 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,974 K.

32 Eridani is divisible in small amateur telescopes. 39 Eridani is a binary star also divisible in small amateur telescopes, 206 light-years from Earth. The primary is an orange-hued giant star of magnitude 4.9 and the secondary is of magnitude 8. 40 Eridani is a triple star system consisting of an orange main-sequence star, a white dwarf, and a red dwarf.

Planetary nebulae are created when a red giant star ejects its outer envelope, forming an expanding shell of gas. However it remains a mystery why these shells are not always spherically symmetrical. 80% of planetary nebulae do not have a spherical shape; instead forming bipolar or elliptical nebulae. One hypothesis for the formation of a non-spherical shape is the effect of the star's magnetic field.

It has an absolute magnitude of −1.55. This is an evolved K-type giant star with a stellar classification of K5 III, which means it has used up its core hydrogen and has expanded. At present it has 40 times the radius of the Sun. It is a variable star of unknown type, with an amplitude of 0.008 in visual magnitude and a period of 4.82 days.

Thuban has a spectral class of A0III, indicating its similarity to Vega in temperature and spectrum, but more luminous and more massive. It has been used as an MK spectral standard for the A0III type. Thuban is not a main sequence star; it has now ceased hydrogen fusion in its core. That makes it a white giant star, being 120 times more luminous than the Sun.

This is a B-type bright giant star with a stellar classification of B8 II. It is a Mercury-Manganese star, showing an overabundance of these elements in its spectrum. The mean longitudinal magnetic field strength is . The star has about four times the mass of the Sun and is radiating 490 times the Sun's luminosity from its photosphere at an effective temperature of 13,500 K.

Phi1 Cancri, Latinized from φ1 Cancri, is a solitary, orange-hued star in the constellation Cancer. It is faintly visible to the naked eye with an apparent visual magnitude of +5.57. Based upon an annual parallax shift of 8.74 mas, it is approximately 370 light years from the Sun. This is an evolved K-type giant star with a stellar classification of K5 III.

The system has an absolute magnitude of −0.14. The magnitude 4.92 primary, designated component A, is an aging giant star with a stellar classification of K3III. The luminosity class of III typically indicates that the star has exhausted the supply of hydrogen at its core, then cooled and expanded off the main sequence. At present it has 25 times the radius of the Sun.

Delta Scuti (δ Sct, δ Scuti) is a giant star in the southern constellation Scutum. With an apparent visual magnitude of 4.72, it is the fifth-brightest star in this small and otherwise undistinguished constellation. Analysis of the parallax measurements made during the Hipparcos mission place this star at a distance of about from Earth. Delta Scuti is the prototype of the Delta Scuti type variable stars.

This object is an aging giant star with a stellar classification of K1 III, which indicates it has exhausted the supply of hydrogen at its core then expanded and cooled off the main sequence. At present it has 22 times the girth of the Sun. It is radiating 182 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,489 K.

This body is moving away from the Sun with a heliocentric radial velocity of +44 km/s. The primary component is an aging K-type giant star with a stellar classification of K0 III. It is a low metallicity star with an iron abundance about half that of the Sun. Keenan and McNeil (1989) found a class of , showing an underabundance of iron in the spectrum.

In 1900, it was 7 minutes of arc north of the equator. As a result of a shift in the Earth's axial tilt, it crossed over to the Southern Hemisphere in December 1923. This is an evolved A-type giant star with a stellar classification of A0 III. It has around three times the mass of the Sun and 4.5 times the Sun's radius.

Alpha Horologii (α Horologii) is a solitary orange-hued giant star in the constellation Horologium. It is visible to the naked eye with an apparent visual magnitude of +3.85. Based upon an annual parallax shift of 28.36 mas as seen from the Earth, it is located from the Sun. The star is moving away from the Sun with a radial velocity of +21.6 km/s.

Gamma Corvi A is a giant star with a stellar classification of B8 III and has approximately 4.2 times the mass of the Sun. It has a blue-white hue. The spectrum of this star displays an anomalously higher than normal abundance of the elements mercury and manganese, making this a Mercury-manganese star. However, there are other elements that show large over or under abundances.

HR 2554, also known as V415 Carinae and A Carinae, is an eclipsing spectroscopic binary of the Algol type in the constellation of Carina whose apparent visual magnitude varies by 0.06 magnitudes and is approximately 4.39 at maximum brightness. Its primary is a G-type bright giant star and its secondary is an A-type main sequence star. It is approximately 553 light years from Earth.

S Microscopii is a star in the constellation Microscopium. It is a red giant star of spectral type M3e-M5.5 that is also a Mira variable, with an apparent magnitude ranging between 7.4 and 14.8 over 210 days. The Astronomical Society of Southern Africa in 2003 reported that observations of S Microscopii were very urgently needed as data on its light curve was incomplete.

OP Andromedae is a variable star in the constellation Andromeda. Varying between magnitudes 6.27 and 6.41 over 2.36 days, it has been classified as an RS Canum Venaticorum variable, but there has not been any proof of binarity, yet. It's a red giant star which spectral classification is K1III. OP Andromedae is one of the few red giant stars where it was detected an overabundance of 7Li.

77 Ceti is a single, orange-hued star located 489 light years away in the equatorial constellation of Cetus. It is faintly visible to the naked eye, having an apparent visual magnitude of 5.7. This is an evolved giant star with a stellar classification of K2 III. It is radiating 187 times the Sun's luminosity from its photosphere at an effective temperature of 4,206 K.

Hall et al. (1995) made additional measurements, finding an orbital period of 80.9 days and an eccentricity that is statistically indistinguishable from zero. The visible component is an evolved giant star with a stellar classification of K0 IIIe, showing strong emission lines. It is an RS Canum Venaticorum variable and its brightness varies by 0.14 magnitudes with a period of 82.9 days due to starspots.

Psi3 Aurigae, Latinized from ψ3 Aurigae, is a single, blue-white hued star in the northern constellation of Auriga. It is dimly visible to the naked eye with an apparent visual magnitude of +5.20. Based upon an annual parallax shift of as seen from the Earth, it is approximately distant from the Sun. This is a B-type giant star with a stellar classification of B8 III.

Epsilon Leporis, Latinized from ε Leporis, is a third-magnitude star in the southern constellation Lepus. The apparent visual magnitude of +3.166 places it third in brightness among the stars in this constellation. Based upon parallax measurements, it is located at a distance of around from Earth. This is an evolved giant star with a stellar classification of K4 III that has expanded to 40 times the Sun's radius.

This is an orange-hued K-type giant star with a stellar classification of K2/3 III. It has about 146% of the mass of the Sun, but at an estimated age of 9.7 billion years it has evolved and expanded to over 25 times the Sun's radius. As a consequence, it shines with around 229 times the solar luminosity. The effective temperature of the star's outer atmosphere is 4,235 K.

Kappa2 Ceti (κ2 Ceti), is a solitary, yellow-hued star located in the equatorial constellation of Cetus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.66. Based upon an annual parallax shift of 10.11 mas as seen from Earth, it is located about 320 light years from the Sun. This is an evolved G-type giant star with a stellar classification of G8 III.

This is a probable astrometric binary, based upon proper motion data collected during the Hipparcos mission. The visible component shows the spectrum of an evolved K-type giant or bright giant star with a stellar classification of K0 II-III. The measured angular diameter, after correction for limb darkening, is . At an estimated distance of this star, this yields a physical size of about 14 times the radius of the Sun.

Omega Virginis (ω Vir, ω Virginis) is a solitary star in the zodiac constellation Virgo. It has an apparent visual magnitude of +5.22, which is bright enough to be faintly visible to the naked eye. Based upon an annual stellar parallax shift of 6.56 milliarcseconds, it is located about 500 light years from the Sun. This is a red giant star with a stellar classification of M4 III.

The star is drifting further from the Earth with a heliocentric radial velocity of +15.2 km/s. It is located near the ecliptic and thus is subject to lunar occultations. This is an aging giant/bright giant star with a stellar classification of G8II-III, and is most likely (97% chance) on the horizontal branch. It is around 350 million years old with 3.3 times the mass of the Sun.

In November 2003, a planet was announced orbiting the giant star. A doppler spectrometer was used to look for effects on the star caused by the gravitational tug of the orbiting planet. Using the amplitude from the radial velocity method, he calculated the planetary mass as 5.25 Jupiter masses and with period 303 days. However that mass is only a minimum because the inclination of the orbit is not known.

7 Draconis, also named Tianyi , is a single star in the northern circumpolar constellation of Draco. It is visible to the naked eye as a faint orange-hued star with a stellar classification of 5.43. Based upon an annual parallax shift of as seen from the Earth, the star is located approximately 780 light- years from the Sun. This is an evolved giant star with a stellar classification of K5 III.

It ranges from magnitudes 5.03 to 6.05. Its designation is from the variable star designation developed by German astronomer Friedrich Wilhelm Argelander. It is a cool star, with estimates of its surface temperature ranging from 2200 to 2700 Kelvin. A giant star, its diameter is 400 times that of the sun, and if placed at the center of the Solar System would stretch out to 30% further than Mars' orbit.

This is an aging red giant star with a stellar classification of M3 III, indicating it has exhausted the hydrogen at its core and evolved off the main sequence. It is a candidate long-period variable star and has been given the designation YY Psc. Its varies in brightness between magnitudes 4.31 and 4.41 with no clear period. Possible periods of 23.1, 32.0, 53.6, and 167.8 days have been identified.

At that distance, the visual magnitude is diminished by an extinction factor of 0.08 due to interstellar dust. This is a red giant star on the asymptotic giant branch, with a stellar classification of M2 III. It is a suspected variable star, although the evidence is considered "doubtful or erroneous". If it does exist, the variability is small with an amplitude of 0.05 magnitude and a timescale of around 30 days.

Delta¹ Tauri A is a single-lined spectroscopic binary with an orbital period of 529.8 days and an eccentricity of 0.42. The visible member, component Aa, is an evolved G- or K-type giant star with a stellar classification of . The 'CN0.5' suffix indicates a mild overabundance of cyanogen in the outer atmosphere. It is chromospherically active and shows a radial velocity variation of with a period of .

This object is an aging giant star with a stellar classification of G9IIIb. Having exhausted the supply of hydrogen at its core, it has cooled and expanded; at present it has 12.3 times the girth of the Sun. The star has an estimated mass about 47% greater than the Sun. It is radiating about 68 times the luminosity of the Sun from its photosphere at an effective temperature of about .

HR 5955 is a single star in the far southern constellation of Apus. It is 28.5 minutes earlier than and about 5 deg. north of the yellow giant star Gamma Apodis, which is the second brightest star in the constellation of Apus. This object has an orange hue and is visible to the naked eye as a dim point of light with an apparent visual magnitude of 5.70.

The secondary is of magnitude 4.0 and has a modest separation, appearing only under intense magnification due to its distance. The northerly star Theta Centauri, officially named Menkent, is an orange giant star of magnitude 2.06. It is the only bright star of Centaurus that is easily visible from mid-northern latitudes. The next bright object is Gamma Centauri, a binary star which appears to the naked eye at magnitude 2.2.

HD 75710 is a single star in the constellation of Vela. It has an apparent visual magnitude of approximately 4.94, which is bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of , it is located about 1,200 light years from the Sun. The stellar classification of this star is A2 III, suggesting it is in the giant star stage of its stellar evolution.

The visible component is an evolved giant star with a stellar classification of K3 III. The interferometry-measured angular diameter of the star, after correcting for limb darkening, is , which, at its estimated distance, equates to a physical radius of about 20 times the radius of the Sun. It is radiating 174 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,050 K.

Epsilon Circini, Latinized from ε Circini, is a solitary star located in the southern constellation of Circinus. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.86. The distance to this star, as determined by a measured annual parallax shift of 8.00 mas, is around 410 light years. This is an evolved K-type giant star with a stellar classification of K2.5 III.

Eta Circini, Latinized from η Circini, is the Bayer designation for a solitary star located in the southern constellation of Circinus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.17. The distance to this star, as determined from an annual parallax shift of 11.82 mas, is around 276 light years. This is an evolved G-type giant star with a stellar classification of G8 III.

OU Andromedae (also HR 9024) is a rotationally variable star in the constellation Andromeda. Varying between magnitudes 5.87 and 5.94, it has been classified as an FK Comae Berenices variable, but the classification is still uncertain. It has a spectral classification of G1IIIe, meaning that it is a giant star that shows emission lines in its spectrum. It is also likely in its horizontal branch phase of evolution.

The primary, Epsilon Hydrae A, is a giant star that is shining with 67 times the luminosity of the Sun. This energy is being radiated from the star's outer atmosphere at an effective temperature of 5,620 K, giving it the yellow hue of a G-type star. It is rotating rapidly with a projected rotational velocity of 19 km s−1. It has an X-ray luminosity of .

This is a single-lined spectroscopic binary system with an orbital period of just 1.71 days in a circular orbit. The unresolved components are close enough that their tidal interaction is significant. The visible component is a slowly pulsating B-type star with a stellar classification of B7III. This implies it is an evolved giant star, but it is actually more likely to be on the main sequence.

Sh2-9, also called Gum 65 is combination emission and reflection nebula in the Scorpius constellation, surrounding the multiple star system Sigma Scorpii. The nebula is a few arcminutes to the northeast to Messier 4, and can be easily seen by small telescopes. Sharpless 9 is a red emission nebula that surrounds the star Sigma Scorpii. It is thought the star Sigma Scorpii, a variable giant star, is ionizing this region.

There is uncertainty about the stellar classification of this star. It has the nominal classification of B9.5IIIe, a B-type giant star with emission lines. However, it has also been classified as an A0 II-IIIe star and as a Herbig Ae/Be star. 51 Ophiuchi is about 300,000 years old with 3.3 times the mass of the Sun and a polar radius 5.7 times the Sun's radius.

Iota Cancri is a wide double star. The primary is a yellow-hued G-type bright giant star of magnitude 4.0, located 330 ± 20 light-years from Earth. It spent much of its stellar life as a B-type main sequence star before expanding and cooling to its current state as it spent its core hydrogen. The secondary is a white main sequence star of spectral type A3V and magnitude 6.57.

Another star visible to the naked eye is γ Capricorni, sometimes called Nashira ("bringing good tidings"); it is a white-hued giant star of magnitude 3.7, 139 light-years from Earth. π Capricorni is a double star with a blue-white hued primary of magnitude 5.1 and a white-hued secondary of magnitude 8.3. It is 670 light-years from Earth and the components are distinguishable in a small telescope.

The brighter star has a stellar classification of B7 III-IV, with the luminosity class of III-IV suggesting that it may lie in an intermediate stage between a subgiant and a giant star. The faint companion is a K-type main sequence star with a classification of K0 V. It has a visual magnitude of 12.5 and an angular separation of 15 arcseconds from the brighter member.

One more source was attributed to a possible cluster K0 giant star member, which was later confirmed to be a cluster member. Three of these sources were identified as binary stars, from a total of six known to exist in the cluster. The luminosity of the sources was typical of RS Canum Venaticorum variables, close binaries that could retain very active coronal sources despite the age of the cluster.

HD 104304 (24 G. Virginis) is a binary star in the zodiac constellation Virgo. It has an apparent magnitude of 5.54, making it visible to the unaided eye under suitable viewing conditions. The stellar classification of G8 IV means that this is a subgiant star that has left the main sequence and has begun to evolve into a giant star. In 2007, a candidate planet was announced orbiting this star.

This is a single-lined spectroscopic binary star system with an orbital period of 258.48 days and an eccentricity of 0.21. The primary, component A, is an evolved K-type giant star with a stellar classification of K0 III. It is a suspected barium star, which may indicate the orbiting companion, component B, is a white dwarf star. The measured angular diameter of the primary, after correction for limb darkening, is .

The star is a member of the thin disk population of the Milky Way galaxy. This is an evolved giant star of type G with an estimated age of 660 million years and a stellar classification of . The suffix notation indicates the spectrum shows a mild underabundance of iron in the outer atmosphere. It has about 2.16 times the mass of the Sun and 7.81 times the Sun's girth.

The star is moving closer to the Earth with a heliocentric radial velocity of −30 km/s, and is predicted to come to within in around 4.4 million years. This is an aging giant star with a stellar classification of G8 IIIa. It is uncertain whether this star is on the red giant branch or the horizontal branch; Reffert et al. (2015) give 57% odd that it is the latter.

The spectrum of this star matches a stellar classification of F0 III, with the luminosity class of III indicating this is most likely an evolved giant star. The variability of this star was discovered by Michel Breger in 1969. It was revealed to be a Delta Scuti-type pulsating variable star with at least two periods of pulsation. The known periods have frequencies of 6.68 and 7.12 cycles per day.

The primary component is a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.1189. The visible member is an aging K-type giant star with a stellar classification of ; sometimes just given as K3 III. The notation of the former class indicates weak lines of CN in the spectrum. This star is an estimated five billion years old with 1.30 times the mass of the Sun.

63 Aurigae is a single star located around 395 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a faint, orange-hued star with an apparent magnitude of 4.91. It is moving closer to the Earth with a heliocentric radial velocity of −28 km/s. This is an evolved giant star with a stellar classification of K4 III.

This is a blue giant star with a stellar classification of B2 III;, a massive star that has evolved off the main sequence. It is around 22.5 million years old with a relatively low projected rotational velocity of 10 km/s. The star has 10 times the mass of the Sun and is radiating 1,622 times the Sun's luminosity from its photosphere at an effective temperature of 17,400 K.

It is moving away from the Earth with a heliocentric radial velocity of +25 km/s. This is classified as an K-type giant star, having evolved off the main sequence after exhausting the hydrogen at its core and expanded to 64 times the Sun's radius. The star is radiating 848 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,910 K.

39 Arietis is a giant star with a stellar classification of K1.5 III. It is currently at an evolutionary stage known as the red clump, indicating that it is generating energy through the fusion of helium at its core. It has 1.6 times the mass of the Sun, but its outer envelope has expanded to around 11 times the Sun's radius. It shines with 56 times the luminosity of the Sun.

Zeta Cygni (ζ Cyg) is a binary star system in the northern constellation of Cygnus, the swan. It has an apparent visual magnitude of 3.26 and, based upon parallax measurements, is about away. The primary component, ζ Cyg A is a giant star with a spectral type of G8 IIIp. Its most likely status is as a red clump giant, an evolved star that has begun core helium fusion.

The light from this system displays an unusually high level of polarization due to interstellar dust. This is a single-lined spectroscopic binary with an orbital period of and a large eccentricity of 0.83. The primary member, designated component A, is an aging giant star with a stellar classification of K2 III. As a consequence of exhausting the hydrogen at its core, it has expanded to 23 times the Sun's radius.

This is an evolved K-type giant star, currently on the red giant branch, with a stellar classification of K4 III and an estimated age of 10 billion years. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified. It has around 1.2 times the mass of the Sun and has expanded to 22 times the Sun's girth.

Upsilon Aurigae, Latinized from υ Aurigae, is the Bayer designation for a star in the northern constellation of Auriga. It has an apparent visual magnitude of 4.74, which means it is bright enough to be seen with the naked eye. Based upon parallax measurements made during the Hipparcos mission, this star is approximately distant from the Earth. This is an evolved red giant star with a stellar classification of M0 III.

This 2.9 billion year old object is an aging giant star with a stellar classification of K2 III. After exhausting the hydrogen at its core, this star evolved off the main sequence and has now expanded to 28 times the Sun's radius. It has 1.47 times the mass of the Sun and is radiating 258 times the Sun's luminosity from its swollen photosphere at an effective temperature of 4,361 K.

Components of the γ Andromedae system (not to scale) γ1 Andromedae (A component) is a bright giant star with a spectral classification of K3IIb. It has an apparent visual magnitude of approximately 2.26. γ2 Andromedae (BC component), with an overall apparent visual magnitude of 4.84, is 9.6 arcseconds away from γ1 Andromedae at a position angle of 63 degrees. γ1 and γ2 have an orbital period of approximately 5,000 years.

The visible component of this system is an aging giant star with a stellar classification of K2 III, which indicates it has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. At present it has nearly sixteen times the girth of the Sun. It is radiating 96 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,535 K.

Chi Virginis b (also known as HD 110014 b) is an extrasolar planet which orbits the K-type giant star Chi Virginis, located approximately 294 light years away in the constellation Virgo. This planet has mass at least 11 times that of Jupiter and takes 835 days to orbit the star twice the distance as Earth from the Sun. This planet was discovered in July 2009 using the radial velocity method.

Chi Piscium (χ Piscium) is a solitary, orange-hued star in the zodiac constellation of Pisces. It can be seen with the naked eye, having an apparent visual magnitude of +4.64. Based upon an annual parallax shift of 8.50 mas as seen from Earth, it is located about 384 light years from the Sun. This is an evolved G-type giant star with a stellar classification of G8.5 III.

17 Monocerotis is a single star located around 490 light years away from the Sun in the equatorial constellation of Monoceros. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.77. The star is moving away from the Earth with a heliocentric radial velocity of +46 km/s. This is an aging giant star with a stellar classification of K4 III.

20 Monocerotis is a single star located about 194 light years away from the Sun in the equatorial constellation of Monoceros. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.92. The star is receding from the Earth with a heliocentric radial velocity of +78 km/s. This object is an aging giant star with a stellar classification of K0 III.

The absolute magnitude of this star is −0.82. This object is an aging red giant star with a stellar classification of M0 III, having exhausted the supply of hydrogen at its core then cooled and expanded. At present it has around 61 times the radius of the Sun. It is a suspected variable star of unknown type, with a brightness that has been measured ranging from 4.94 down to 4.98.

This is an evolved G-type giant star with a stellar classification of . The suffix notation indicates there is a strong underabundance of iron in the spectrum, and an overabundance of cyanogen (CN). ε Andromedae is believed to be a red clump star which is fusing helium in its core. It has about the same mass as the Sun, but has expanded to nine times the Sun's radius.

R Lyrae near Vega R Lyrae is a 4th magnitude semiregular variable star in the constellation Lyra, approximately 350 light years away from Earth. It is a red giant star of the spectral type M5III, meaning it has a surface temperature of under 3,500 kelvins. It is much larger and brighter, yet cooler, than the Sun. In the near-infrared J band, it is brighter than the nearby Vega.

This is an aging giant star with a stellar classification of K2III, which indicates it has exhausted the supply of hydrogen at its core, then evolved away from the main sequence by cooling and expanding. At present it has 20 times the radius of the Sun. The star is radiating 128 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,325 K.

Alpha Antliae (Alpha Ant, α Antliae, α Ant) is the brightest star in the constellation of Antlia but it has not been given a proper name. It is approximately 320 light-years from the Solar System. It is a K-type giant star with an apparent visual magnitude of 4.25. This star has 2.2 times the mass of the Sun and has expanded to 41 times the solar radius.

It has an absolute magnitude of −1.45. This is an aging K-type giant star with a stellar classification of K4III, having exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. At present it has about 60 times the radius of the Sun and is radiating 769 times the Sun's luminosity from its swollen photosphere at an effective temperature of 3,940 K.

This is an evolved K-type giant star with a stellar classification of K3 III, having exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. It has about 2.4 times the mass of the Sun and has expanded to 22.3 times the Sun's radius. The star is radiating 155 times the Sun's luminosity from its photosphere at an effective temperature of 4,269 K.

This is an aging giant star with a stellar classification of K2IIIab. It is a red clump giant, meaning it on the horizontal branch and is generating energy through helium fusion at its core. The star is roughly six billion years old with slightly more mass than the Sun. With the supply of hydrogen at its core exhausted, it has expanded to nearly 12 times the Sun's radius.

6 Corvi is a single star in the southern constellation of Corvus, located 341 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.66. This object is moving closer to the Earth with a heliocentric radial velocity of −2.4 km/s. It is an evolved giant star with a stellar classification of K1 III.

Nu Aquarii (ν Aqr, ν Aquarii) is the Bayer designation for a star in the equatorial constellation of Aquarius. With an apparent visual magnitude of 4.52, Nu Aquarii is visible to the naked eye. Its distance from Earth, as determined from parallax measurements, is around . At an estimated age of 708 million years, it has evolved into a giant star with a spectrum that matches a stellar classification of G8 III.

At an estimated age of 254 million years, this appears to be an evolved B-type giant star with a stellar classification of B9 III. It is a mercury-manganese chemically peculiar star, indicating the spectrum shows abnormal abundances of these elements. The star has about four times the radius of the Sun and it radiates 173 times the Sun's luminosity from its photosphere at an effective temperature of 10,152 K.

This is an aging giant star with a stellar classification of K2 IIIa, having already consumed the hydrogen at its core and evolved away from the main sequence. It has nearly five times the mass of the Sun but has expanded to around 100 times the Sun's radius. The star is radiating 2,889 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,200 K.

This is a single- lined spectroscopic binary system, but the secondary has been detected using interferometry. It is a RS Canum Venaticorum variable system with eclipses. The total amplitude of variation is only about a thousandth of a magnitude. The secondary star is similar to the sun, presumably a main sequence star, while the primary is a giant star 25 times larger than the sun and two hundred times more luminous.

This is an aging giant star with a stellar classification of K0 III, having exhausted the supply of hydrogen at its core then cooled and expanded to almost ten times the Sun's radius. It is nearly two billion years old with 1.76 times the mass of the Sun. The star is radiating 43 times the luminosity of the Sun from its photosphere at an effective temperature of 4,707 K.

It is a member of the Arcturus moving group. This is an evolved K-type giant star on the asymptotic giant branch with a stellar classification of K5 III. With the supply of hydrogen at its core exhausted, it has expanded and now spans 29.6 times the radius of the Sun. It is radiating 200 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,990 K.

Gamma Microscopii (γ Microscopii, γ Mic) is the brightest star in the faint southern constellation of Microscopium. It has an apparent visual magnitude of 4.68, which is too dim to be viewed from city skies. The distance to this star has been determined using parallax measurements made with the Gaia telescope, which place it at . Based upon a stellar classification of G6 III, this is a G-type giant star.

It is a member of the Ursa Major Moving Group of co-moving stars. π1 Pegasi (right) and π2 Pegasi (left) in optical light The visible component is an aging giant star with a stellar classification of G8IIIb. It has a high rate of spin, with a projected rotational velocity of 135 km/s. This is giving it an equatorial bulge that is 17% larger than the polar radius.

HD 122430 b is a proposed giant planet orbiting around the giant star HD 122430. It has a mass at least 3.71 times that of Jupiter. This planet located at a distance of 1.02 astronomical units away from its star, which is very similar to the Earth's distance from the Sun. Despite of this, the higher luminosity of the star implies it is heated much more strongly than the Earth is.

This is a probable astrometric binary system. The visible component, Omicron Piscium A, is an evolved K-type giant star with a stellar classification of K0 III. At the estimated age of 390 million years, it is most likely (76% chance) on the horizontal branch, rather than the red- giant branch. As such, it is a red clump star that is generating energy through helium fusion at its core.

NGC 2423-3 is a red giant star approximately 2498 light-years away in the constellation of Puppis. The star is part of the NGC 2423 open cluster (hence the name NGC 2423-3). The star has an apparent magnitude of nine and an absolute magnitude of zero, with a mass of 2.4 times the Sun. As of 2007, it has been confirmed that an extrasolar planet orbits the star.

Upsilon² Eridani (υ² Eridani, abbreviated Upsilon² Eri, υ² Eri), officially named Theemin , is a star in the constellation of Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.8. Based upon parallax measurements obtained during the Hipparcos mission, it is approximately 66 parsecs (214 light-years) from the Sun. This is an evolved red clump giant star with a stellar classification of G8+ III.

The two components of the binary system includes a K-type giant star and a G-type main sequence star. The primary star is estimated to be 1.8 times as massive and 13 times the diameter of the Sun. The secondary star is estimated to be similar to the Sun in size and mass. They orbit their common barycenter in a period precisely estimated to be 24.64877 days.

Delta Draconis is a giant star with a stellar classification of G9 III. This indicates that, at an estimated age of 800 million years, it has exhausted the supply of hydrogen at its core and entered a later stage in its evolution. The angular diameter of the star is estimated as . At a parallax of 32.54 mas, this corresponds to a physical radius equal to 11 times the solar radius.

It is moving closer to the Earth with a heliocentric radial velocity of −23 km/s. Houk (1978) assigned the spectral classification of this star as F1III, which suggests it is an F-type (yellow- white) star that has evolved away from the main sequence and expanded into a giant. However, Gray et al. (2001) found a class of F0 Ib-II, matching a supergiant/bright giant star.

Kappa Capricorni (κ Cap, κ Capricorni) is a solitary star in the constellation Capricornus. It is visible to the naked eye with an apparent visual magnitude of +4.73. Based upon an annual parallax shift of 11.09 mas as seen from the Earth, the star is located about 294 light years from the Sun. This is a yellow-hued, evolved, G-type giant star with a stellar classification of G8 III.

This is an aging giant star with a stellar classification of K1.5IIIb:, having exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. At present it has 13 times the girth of the Sun, with a near-solar metallicity of −0.01. The star is radiating 70 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,679 K.

Despite having the Bayer designation α Ceti, at visual magnitude 2.54 this star is actually not the brightest star in the constellation Cetus. That honor goes instead to Beta Ceti at magnitude 2.04. Menkar is a red giant with a stellar classification of M1.5 IIIa. It has more than twice the mass of the Sun and, as a giant star has expanded to about 89 times the Sun's radius.

The visible component is an aging giant star with a stellar classification of K1 III and an estimated age of 4.20 billion years old. Having exhausted the supply of hydrogen at its core, the star has expanded to 22 times the Sun's radius. It has 1.55 times the mass of the Sun and is radiating 173 times the Sun's luminosity from its swollen photosphere at an effective temperature of 4,498 K.

Tau4 Eridani (τ4 Eridani, τ4 Eri) is a binary star system in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.65. The distance to this star can be estimated using the parallax method, which yields a value of roughly 300 light years. This is an evolved red giant star currently on the asymptotic giant branch with a stellar classification of M3/4 III.

42 Draconis b (abbreviated 42 Dra b), formally named Orbitar , is an extrasolar planet located approximately 315 light years from Earth in the constellation of Draco. It orbits the 5th magnitude K-type giant star 42 Draconis with a period of 479 days and 38% orbital eccentricity. The planet was discovered using the radial velocity method on March 20, 2009. Following its discovery the planet was designated 42 Draconis b.

Kappa Draconis, Latinized from κ Draconis, is a blue giant star located in the northern circumpolar constellation of Draco. At an apparent magnitude of 3.88, it is barely visible to the naked eye when artificial lighting from cities is present. Nevertheless, it is a powerful star, approximately five time as massive as the Sun. It is about 490 light-years away, and is 1,400 times brighter than the Sun.

Alpha Pyxidis (Alpha Pyx, α Pyxidis, α Pyx) is a giant star in the constellation Pyxis. It has a stellar classification of B1.5III and is a Beta Cephei variable. This star has more than ten times the mass of the Sun and is more than six times the Sun's radius. The surface temperature is 24,300 K and the star is about 10,000 times as luminous as the Sun.

20 Ceti is a single star located around 590 light years away in the equatorial constellation of Cetus. It is faintly visible to the naked eye with apparent magnitude is 4.76. The Bright Star Catalogue has this star classified as M0III, matching an aging red giant star that has consumed the hydrogen at its core and expanded. Houk and Swift (1999) listed an earlier class of K5 III.

This is an astrometric binary system with a period of 6.5 years (2,374 days) and an orbital eccentricity of 0.10. The visible component is an aging giant star of type G with a stellar classification of G9 IIIb Fe−0.5. The suffix notation indicates the spectrum displays a mild underabundance of iron. It has 1.29 times the mass of the Sun and has expanded to 9.3 times the Sun's radius.

HD 15558 A is a spectroscopic binary system containing at least two massive luminous class O stars. The primary is an O4.5 giant star with a surface temperature over 46,800 K. It has a mass of 152 and a luminosity of 660,000 , making it one of the most massive stars in the Milky Way Galaxy. The star loses 1.5×10−5 per year. The secondary is an O7V star.

Pi Eridani, Latinized from π Eridani, is a star in the constellation Eridanus. It has an apparent visual magnitude of 4.40, which is bright enough to be seen on a dark, clear night. Based upon parallax measurements, it is located roughly 480 light years from the Sun. This is an evolved red giant star with a stellar classification of M1 III, and is currently on the asymptotic giant branch.

Epsilon Tauri (ε Tauri, abbreviated Epsilon Tau, ε Tau), formally named Ain , is an orange giant star located approximately 45 parsecs (147 light-years) from the Sun in the constellation of Taurus. An extrasolar planet (designated Epsilon Tauri b, later named Amateru) is believed to be orbiting the star. It is a member of the Hyades open cluster. As such its age is well constrained at 625 million years.

It is a suspected member of the Sirius stream of co- moving stars. This is an evolved G-type giant star with a stellar classification of G8 III. It is a red clump star, which means it is on the horizontal branch and generating energy through the thermonuclear fusion of hydrogen at its core. The star is emitting X-rays with a luminosity of in the 0.3–10 keV band.

This is an orange-hued K-type giant star on the red giant branch, with a stellar classification of K2 III. It has an estimated 1.75 times the mass of the Sun but after evolving away from the main sequence it has expanded to 9.8 times the Sun's radius. The star is radiating 39 times the solar luminosity from its photosphere at an effective temperature of 4,605 K.

Nu Ursae Majoris (ν Ursae Majoris, abbreviated Nu UMa, ν UMa), formally named Alula Borealis , is a double star in the northern circumpolar constellation of Ursa Major. At an apparent visual magnitude of +3.490, it is bright enough to be seen with the naked eye. Based upon parallax measurements, the distance to ν Ursae Majoris is about . This is a giant star with a stellar classification of K3 III.

R Normae is a Mira variable star located near Eta Normae in the southern constellation of Norma. This is an intermediate-mass red giant star that is generating part of its energy through hydrogen fusion. Because this fusion is thought to be occurring under conditions of convection, it is generating an excess of lithium. The star ranges from magnitude 6.5 to 12.8 and has a relatively long period of 496 days.

It is drifting further away with a radial velocity of +13.3 km/s. This object is an aging bright giant star with a stellar classification of G6IIb With the supply of hydrogen at its core exhausted, it has expanded to 12 times the radius of the Sun. The star is radiating 89 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 5,197 K.

Iota Tucanae (ι Tuc, ι Tucanae) is a solitary star in the southern constellation of Tucana. Based upon an annual parallax shift of 10.72 mas as seen from Earth, it is located around 304 light years from the Sun. With an apparent visual magnitude of +5.33, it is faintly visible to the naked eye. This is a yellow-hued G-type giant star with a stellar classification of G5 III.

HD 155035 is the Henry Draper Catalogue designation for a star in the constellation Ara, the Altar. It is located at a distance of approximately from Earth and has an apparent visual magnitude of 5.92, making it is faintly visible to the naked eye. This is a red giant star with a stellar classification of M1.5 III. It an irregular variable that changes brightness over an amplitude range of 0.12 magnitudes.

69 Ceti is a single star located around 860 light years away in the equatorial constellation of Cetus. It is visible to the naked eye with an apparent visual magnitude of 5.3. This is an aging red giant star with a stellar classification of M1/2III. It is radiating 1,813 times the Sun's luminosity from an enlarged photosphere, 100 times the Sun's radius, at an effective temperature of 3,765 K.

Its common name comes from the Arabic phrase for "ox- driver". It is 219 light-years away and has a luminosity of . Located 86 light-years distant, Gamma Boötis, or Seginus, is a white giant star of spectral class A7III, with a luminosity 34 times and diameter 3.5 times that of the Sun. It is a Delta Scuti variable, ranging between magnitudes 3.02 and 3.07 every 7 hours.

HR 6902 (also designated V2291 Oph) is a binary system located 790 light years away from the Sun in the Ophiuchus constellation. The system includes an orange bright giant star and a B-type main sequence star, forming an eclipsing binary of Zeta Aurigae type. The system is also surrounded by a warm circumstellar envelope and the spectra show silicon and carbon absorption up to a distance of 3.3 giant radii.

This object is an aging red giant star on the asymptotic giant branch with a stellar classification of M4IIIa. Its variable nature was discovered by American astronomer J. Ashbrook in 1948. This is a suspected slow irregular variable of sub-type Lb that varies in visual magnitude from 4.80 down to 4.96. Long-term photometry measurements suggest there are at least four pulsation periods ranging from 27.1 to 39.0 days.

Alpha Lyncis (α Lyn, α Lyncis) is the brightest star in the northern constellation of Lynx with an apparent magnitude of +3.13. Unusually, it is the only star in the constellation that has a Bayer designation. Based upon parallax measurements, this star is located about from the Earth. This is a giant star that has exhausted the hydrogen at its core and has evolved away from the main sequence.

Located 163 ± 4 light-years away, it is an orange giant star of spectral type K0III that is 1.0–1.4 times as massive as the Sun. An ageing star, it has cooled and expanded to times the Sun's radius. It is radiating as much power as the Sun from its outer envelope at an effective temperature of . Traditionally called Alkes "the cup", and marking the base of the cup is Alpha Crateris, an orange- hued star of magnitude 4.1, that is 141 ± 2 light-years from the Sun. With an estimated mass 1.75 ± 0.24 times that of the Sun, it has exhausted its core hydrogen and expanded to 13.2 ± 0.55 times the Sun's diameter, shining with 69 times its luminosity and an effective temperature of around 4600 K. With a magnitude of 4.5, Beta Crateris is a binary star system, consisting of a white-hued giant star of spectral type A1III and a white dwarf of spectral type DA1.4, 296 ± 8 light-years from the Sun.

AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日 Mu Ceti is an A9 giant star. It has been suspected to be a δ Scuti variable, but most studies find it to be of constant brightness. Three companions were all discovered during occultations of Mu Ceti by the Moon. An orbit was derived for the brightest with a period of 1202 days.

The primary component, η Sagittarii A, is a red giant star with a stellar classification of M2 III. It is an evolved star that is currently at a stage called the asymptotic giant branch, having exhausted both the hydrogen and the helium at its core. This star is classified as an oxygen-rich irregular variable, as it undergoes small magnitude fluctuations between +3.08 and 3.12. The measured angular diameter of this star is .

Rho2 Sagittarii (ρ2 Sagittarii) is a star in the zodiac constellation of Sagittarius. With an apparent visual magnitude of +5.87, it is near the lower limit of stars that can be seen with the naked eye. Based upon an annual parallax shift of 9.82 mas as seen from Earth, it is located around 330 light years from the Sun. This is an evolved K-type giant star with a stellar classification of K0 III.

Iota Volantis, Latinized as ι Volantis, is the Bayer designation for a star in the southern constellation of Volans. It has an apparent visual magnitude of 5.39, which indicates it is faintly visible to the naked eye. With a parallax of 0.00579″, it lies at an estimated distance of roughly 560 light years from the Sun. This star has a stellar classification of B7 III, which means it is a B-type giant star.

The spectrum of Xi2 Sagittarii yields a mixed stellar classification of G8/K0 II/III, showing traits of a G- or K-type giant or bright giant star. It has an estimated 3.36 times the mass of the Sun and about 14 times the Sun's radius. At an age of around 380 million years, it is radiating 676 times the Sun's luminosity from its photosphere at an effective temperature of 4,541 K.

This is an evolved, K-type giant star with a stellar classification of K3 III. It is a suspected optical variable star with a magnitude range of 5.42 to 5.46. At infrared wavelengths, it shows large amplitude variation with a period of 505 days. The star has expanded to about 37 times the Sun's radius and is radiating 301 times the solar luminosity from its photosphere at an effective temperature of 4,040 K.

It is moving closer to the Sun with a radial velocity of −17 km/s. This is a single-lined spectroscopic binary with an orbital period of and a high eccentricity of 0.713. The visible component has a stellar classification of G8 IIIa, indicating it is an evolved G-type giant star. It is a probable red clump star, which would mean it is generating energy through helium fusion at its core.

Messier 7 (M7), with V957 Scorpii the bright star to the right of the central square Messier 7 is a naked-eye open cluster. Except for one obvious orange giant star, its brightest members are mostly early A and late B main sequence stars and giants. Several of them are also chemically peculiar stars. However, two stars are hotter than the others and lie to the left of the isochrone for the cluster.

It is located at a distance of approximately 283 light years from the Sun based on parallax, and is drifting further away with a radial velocity of 49 km/s. At that distance, the visual brightness of this star is diminished by an extinction of 0.174 due to interstellar dust. The star has an absolute magnitude of 0.95. This is an aging giant star on the horizontal branch with a stellar classification of K1.5III CN1.

Its two brightest stars, Delta Crateris of magnitude 3.56 and Alpha Crateris of magnitude 4.07, are ageing orange giant stars that are cooler and larger than the Sun. Beta Crateris is a binary star system composed of a white giant star and a white dwarf. Seven star systems have been found to host planets. A few notable galaxies, including Crater 2 and NGC 3981, and a famous quasar lie within the borders of the constellation.

The primary, component A, is a magnitude 4.95 evolved giant star with a stellar classification of G8 III. It is a red clump star that is generating energy through the fusion of helium at its core. Zeta Crateris has expanded to 13 times the radius of the Sun, and shines with 157 times the luminosity of the Sun. Online data (HIP number needed) The secondary, component B, is a magnitude 7.84 star.

The system is located 179 (±4) light-years from the earth. At magnitude 5.0, Beta Horologii is a white giant 63 times as luminous as the Sun with an effective temperature of 8,303K. It is 312 (±4) light-years from Earth, and has been little-studied. Lambda Horologii is an ageing yellow-white giant star of spectral type F2III that spins around at 140km/second, and is hence mildly flattened at its poles (oblate).

Albireo, designated Beta Cygni, is a celebrated binary star among amateur astronomers for its contrasting hues. The primary is an orange-hued giant star of magnitude 3.1 and the secondary is a blue-green hued star of magnitude 5.1. The system is 380 light- years away and is visible in large binoculars and all amateur telescopes. Gamma Cygni, traditionally named Sadr, is a yellow-tinged supergiant star of magnitude 2.2, 1500 light-years away.

However, Morbey and Griffin (1987) later cast some doubt on the validity of these results, suggesting that further review is needed. The visible member of this system, component A, is an evolved F-type giant star with a stellar classification of F5 III. It has an estimated 1.78 times the mass of the Sun and 2.8 times the Sun's radius. The star is spinning with a projected rotational velocity of 17 km/s.

This object is an aging K-type giant star with a stellar classification of K1III. It is classified as a red clump giant, suggesting it is on the horizontal branch undergoing core helium fusion. The star has 2.7 times the mass of the Sun and has expanded to 11 times the Sun's radius. It is radiating 67 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 5,060 K.

Gamma Chamaeleontis, Latinized from γ Chamaeleontis, is a solitary star located in the southern circumpolar constellation of Chamaeleon. It can faintly be seen with the naked eye on a dark night, having an apparent visual magnitude of 4.12. Based upon an annual parallax shift of 7.81 mas, it is located around 418 light years from the Sun. This is an evolved K-type giant star with a stellar classification of K5 III.

This object is an aging G-type giant star with a stellar classification of G6/8 III. Having exhausted the supply of hydrogen at its core, the star has cooled and expanded until now it has 11 times the girth of the Sun. It is a suspected variable star of unknown type. The star is radiating 71 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,967 K.

Delta Coronae Australis is a single star located in the southern constellation of Corona Australis. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.57. The star is located about 174 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +21 km/s. This object is an evolved giant star with a stellar classification of K1III.

HD 1690 is an evolved K-type giant star. Its age is estimated at 6.7 billion years (two billion years older than the Sun) and its radius is given at 16.7 solar radii. Its metallicity is 30% that of the sun. The Hipparcos parallax data have resulted in a distance determination of just , but more recent data from Gaia data have placed HD 1690 much farther from the Sun at .GaiaSource-2429846549069734784-2430330987021111936.

Hamal , designation Alpha Arietis (α Arietis, abbreviated Alpha Ari, α Ari), is the brightest star in the northern zodiacal constellation of Aries. With an apparent visual magnitude of 2.0, it is the mean 50th brightest star in the night sky. Based upon parallax measurements made with the Hipparcos astrometry satellite, Hamal is about from Earth. It is a giant star that may host an orbiting planet with a mass greater than Jupiter.

This is an evolved, cool red giant star with a stellar classification of class M5III. It is a semiregular variable with a magnitude range of 4.58 to 5.3 and a (poorly defined) period around 55 days. The star has 1.34 times the mass of the Sun and has expanded to around 112 times the Sun's radius. It is radiating 1,819 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,560 K.

Rho Ursae Majoris (ρ UMa) is the Bayer designation for a solitary star in the northern circumpolar constellation of Ursa Major. It is faintly visible to the naked eye with an apparent visual magnitude of 4.74. The distance to this star, based upon an annual parallax shift of 10.37 mas, is around 315 light years. With a stellar classification of M3 III, this is a red giant star on the asymptotic giant branch.

Griffin (2012) found this to be a single-lined spectroscopic binary system with an orbital period of and an eccentricity of 0.23. The a sin i value for the primary component is , where a is the semimajor axis and i is the (unknown) orbital inclination. This value provides a lower bound for the actual semimajor axis. The visible component is an evolved K-type giant star with a stellar classification of K5 III.

11 Ursae Minoris is a single star located approximately 410 light years away in the northern circumpolar constellation of Ursa Minor. The star is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.15. It is moving closer to the Earth with a heliocentric radial velocity of −17.5 km/s. This is an aging K-type giant star with a stellar classification of K4 III.

It is an ellipsoidal variable, which means the orbit is sufficiently close that the shapes of the components are being distorted by their mutual gravitation. This is causing the visual magnitude of the system to vary regularly by 0m.05 over the course of each orbit, as the orientation of the stars change with respect to the Earth. The primary component is a B-type giant star with a stellar classification of B2 III.

This is an evolved K-type giant star on the horizontal branch, with a stellar classification of K0/1 III. It is a suspected variable star with a measured variation between 4.45 and 4.49 in visual magnitude. Pi6 Orionis has over four times the mass of the Sun and has expanded to around 88 times the Sun's radius. Over the course of its life span, the star has shed around solar masses.

With a stellar classification of K3 III, Rho Draconis is a normal giant star that is past the first dredge-up phase of its post-main sequence evolution. It has the peculiar spectrum of a CN star, showing abnormal line strengths for cyanogen and calcium. The star has expanded to around 28 times the Sun's radius and it is radiating 402 times the solar luminosity from its photosphere at an effective temperature of 4,370 K.

Upsilon Piscis Austrini (υ Piscis Austrini) is a solitary, orange-hued star in the southern constellation of Piscis Austrinus. It is faintly visible to the naked eye with an apparent visual magnitude of +4.98. Based upon an annual parallax shift of 7.69 mas as seen from the Earth, the star is located 420 light-years from the Sun. This is an evolved K-type giant star with a stellar classification of K4 III.

This object is an aging giant star with a stellar classification of K4+ III. A 1993 study found that it varied in brightness by 0.05 magnitude over 25 to 30 days. It is classified as a semiregular variable with a brightness that ranges from 4.21 to as low as 4.27, and has the variable star designation BN Lyncis. 31 Lyncis is 1.3 billion years old with almost double the mass of the Sun.

Nu Aurigae, Latinized from ν Aurigae, is the Bayer designation for a star in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of 3.96 and is approximately distant from the Earth. This is an evolved giant star with a stellar classification of G9.5 III. It is a red clump star, which indicates that it is generating energy through the fusion of helium at its core.

To small telescopes, Theta Muscae appears as a double star, with a blue-cream brighter star and an O9III companion of magnitude 7.3 some 5.3 arcseconds away. The primary θ Muscae A is a massive triple star system. The companion θ Muscae B is not part of the triple system but an optical double which happens to be along the same line of sight. It is a luminous O class giant star.

At that distance, its brightness is diminished by 0.21 in magnitude from extinction caused by interstellar gas and dust. This is a suspected spectroscopic binary with an angular separation of between the two components. The visible component is an evolved giant star with a stellar classification of K1 III. It is a suspected variable star of unknown type, and is around 2.6 billion years old with 1.6 times the mass of the Sun.

The brightness of the star is diminished by 0.15 in magnitude from extinction caused by interstellar gas and dust. The star is positioned near the ecliptic and thus is subject to lunar occultations. This is an aging red giant star with a stellar classification of M0 III that is currently evolving along the asymptotic giant branch. Having exhausted the supply of hydrogen at its core, the star has expanded to 41 times the Sun's radius.

The system is moving closer to the Earth with a heliocentric radial velocity of −16 km/s. The calculated orbit of the visual binary has a period of 48.65 years and a large eccentricity of 0.868. The primary, component A, is itself a single-lined spectroscopic binary with a period of 5.8839 days and an eccentricity of . One study gives the system a stellar classification of F7 III, suggesting it contains an evolved giant star.

Parallax measurements provide a distance estimate of approximately 570 light years from the Sun. Gray and associates (1989) found a stellar classification of A8 III for this object, matching an evolved A-type giant star. Abt and Morrell (1995) listed a class of F0V, suggesting it is an F-type main-sequence star. It is a Delta Scuti variable whose brightness varies between magnitudes 6.54 and 6.59 with a period of 0.219 days.

The primary is an aging giant star with a stellar classification of . It is 3.9 billion years old with 1.49 times the mass of the Sun and around 44 times the Sun's radius. This star is radiating 561 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,102 K. The suspected companion star should be a white dwarf that previously transferred s-process elements to the visible member.

19 Aurigae is a single star located approximately 3,600 light years away from the Sun in the northern constellation Auriga. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.05. The star is moving closer to the Earth with a heliocentric radial velocity of 4.3 km/s. This is an evolved A-type bright giant star with a stellar classification of A5 II+.

This system is known to have three components. The primary is a giant star with a stellar classification of , meaning that an overabundance of barium ionized one time is observed in the spectrum of the star, making it a barium star. The secondary component is likely a white dwarf with a period of 748.2 days and an eccentricity of 0.34. There is a third component at an angular separation of 0.22 arcseconds.

At that distance, the visual magnitude is diminished by an extinction of 0.18 due to interstellar dust. It is moving closer to the Earth with a heliocentric radial velocity of −9 km/s. Relative to its neighbors, 15 Aqr has a peculiar velocity of and may (62% chance) be a runaway star. Hube (1970) found a stellar classification of B7 III for this star, which would suggest it is a B-type giant star.

This is an astrometric binary system. The primary has a stellar classification of F2 III, suggesting that it is a giant star. Despite being an evolved star with four times the radius of the Sun, it is spinning rapidly with a projected rotational velocity of 139.6 km/s. This is causing a pronounced equatorial bulge, with the radius of the star along the equator being 24% greater than the radius at the poles.

At that distance, the visual magnitude of the star is diminished by an extinction of 0.088 due to interstellar dust. It is moving further from the Earth with a heliocentric radial velocity of +48 km/s. This is an evolved giant star currently on the red giant branch with a stellar classification of K0 III. The star has 1.35 times the mass of the Sun and has expanded to 7.86 times the Sun's radius.

1 Cassiopeiae is a single star in the northern constellation of Cassiopeia, located around 1,130 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of +4.84. This object is moving closer to the Earth with a heliocentric radial velocity of −9 km/s. The stellar classification of 1 Cassiopeiae is B0.5 III, matching an evolved B-type giant star.

The star is a member of the HD 1614 supercluster. This is an evolved red giant star with a stellar classification of M5 III. It is classified as a semiregular variable star and its brightness varies from magnitude +4.16 to +4.26 with a period of 12.57 days. The star has around 70 times the Sun's radius and is radiating 72 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,398 K.

The giant star will eventually become a white dwarf and an exocomet that gets too close to the white dwarf will sublimate or tidal disrupted by the gravity of the white dwarf. This will produce dusty debris around the white dwarf, which is measurable in infrared wavelengths. The material can be accreted by the white dwarf and pollute the atmosphere. This pollution appears in the spectra of a white dwarf as metal lines.

This object is an Ap star with a stellar classification of B9.5IIIspSi matching a late B-type giant star. The 'Si' suffix indicates an abundance anomaly of silicon. It is an Alpha2 Canum Venaticorum variable that ranges from magnitude 4.68 down to 4.73 with a period of 1.89 days – the same as its rotational period. It is 3.65 times as massive and 245 times as luminous as the Sun, with 3.44 times the Sun's diameter.

Sigma Octantis (also written as σ Octantis; abbreviated as Sig Oct or σ Oct), officially named Polaris Australis (), is the current South Star. Its apparent position near the southern celestial pole makes it the pole star of the Southern Hemisphere. This is a solitary star in the southern circumpolar constellation of Octans. Located approximately 281 light-years from Earth, it is classified as a giant star with a spectral type of F0 III.

Estimated to be around 10 billion years old, this is an aging red giant star with a stellar classification of M3.5 III. It is a periodic variable with a frequency of 11.98912 cycles per day and an amplitude of 0.0254 in magnitude. The spectrum does not show evidence of s-process enhancement. 10 Dra has 93% of the mass of the Sun but has expanded to about 83 times the Sun's radius.

The visible component is an aging K-type giant star with a stellar classification of K0+IIIaBa0.2, showing a slight overabundance of barium. The spectrum displays strong violet lines of CN. With the supply of hydrogen at its core exhausted, this star has expanded to 27 times the radius of the Sun. It is radiating 311 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,750 K.

This is an evolved giant star with a stellar classification of K3 III. It is a red clump giant, which means it is on the horizontal branch and is generating energy through helium fusion at its core. At the age of 4.46 billion years, it has 1.25 times the mass of the Sun and is radiating 61.7 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,370 K.

Olin J. Eggen listed it as a probable member of the Hyades supercluster. This is an aging red giant star currently on the asymptotic giant branch with a stellar classification of M2III. It is not longer undergoing core hydrogen fusion and has expanded to 61 times the radius of the Sun. The star is radiating 700 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,797 K.

Epsilon1 Arae (ε1 Ara, ε1 Arae) is the Bayer designation for a star in the constellation Ara, the Altar. It is visible to the naked eye with an apparent visual magnitude of +4.1 Based upon an annual parallax shift of 9.04 mas, this star is around distant from the Earth. ε1 Arae is an evolved giant star with a stellar classification of K3 III. It is around 74% more massive than the Sun.

Iota Arae, Latinized from ι Arae, is the Bayer designation for a star in the southern constellation of Ara. It is approximately from Earth, give or take a 70 light-year margin of error, and has an apparent visual magnitude of 5.25. Based upon the Bortle Dark-Sky Scale, this means the star is visible to the naked eye from suburban skies. This is an evolved giant star with a stellar classification of B2 IIIne.

Although it appears at the edge of the Carina Nebula, it is much closer than the nebula. It is also not considered a member of the nearby Alessi 5 open cluster of stars. This is an aging K-type giant star with a stellar classification of K1III, having exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. At present it has 14 times the radius of the Sun.

Kappa Aquarii is most probably a wide binary star system. The brighter component is a giant star with a stellar classification of K2 III. It has exhausted the supply of hydrogen at its core and has expanded to 13 times the radius of the Sun. It is radiating 60 times the Sun's luminosity from its outer envelope at an effective temperature of 4,581 K, giving it the orange- hued glow of a K-type star.

This object is an evolved K-type giant star with a stellar classification of K0 III. It has exhausted the supply of hydrogen at its core, causing it to cool and expand. At present it has 12 times the radius of the Sun. With 1.9 times the mass of the Sun it is a red clump star, which indicates it is on the horizontal branch generating energy through helium fusion at its core.

With over double the mass of the Sun, this is an evolved giant star that has a stellar classification of K0 III. The measured angular diameter of this star is . At the estimated distance of 98 Aquarii, this yields a physical size of about 14 times the radius of the Sun. The expanded outer envelope has an effective temperature of 4,630 K, giving it the orange glow of a K-type star.

The primary is a giant star with a stellar classification of . It is a Mercury- Manganese star, showing a surfeit of these elements in the spectrum. With five times the Sun's mass, this star is radiating 1,035 times as much luminosity from its outer atmosphere at an effective temperature of 12,593 K. This heat gives it the blue-white hue of a B-type star. The companion may be a variable star.

This is a giant star with a stellar classification of K3 III, which, at the age of 4.58 billion years old, has exhausted the hydrogen at its core and evolved away from the main sequence. The star has 1.32 times the mass of the Sun and has expanded to 24 times the Sun's radius. It is radiating 190.5 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,188 K.

This is an aging giant star with a stellar classification of , most likely (98% chance) on the red giant branch. The suffix notation indicates an underabundance of iron in the spectrum, and some uncertainty about the classification. It is around 8.1 billion years old with 0.88 times the mass of the Sun. As a consequence of exhausting the hydrogen at its core, the star has expanded to 33.4 times the Sun's radius.

This is an aging giant star with a stellar classification of K0 III, which indicates it has exhausted the hydrogen supply at its code and evolved away from the main sequence. It is 324 million years old with three times the mass of the Sun and has expanded to 14 times the Sun's radius. The star is radiating 100 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,915 K.

This is a single-lined spectroscopic binary system with an orbital period of 576 days and an eccentricity of 0.3. The a sin i value for the primary is , where a is the semimajor axis and i is the (unknown) orbital inclination. The provides a minimum value for the actual semimajor axis. The visible component is a red giant star and has been defined as a standard star for the stellar classification of K6 IIIa.

For comparison, the Sun loses (2-3) x 10−14 solar masses per year due to its solar wind, several hundred million times less than WR 30a. The secondary star has an O5 spectral class. It is not a supergiant, but could be a main sequence or giant star. Some helium lines and nitrogen emission is detected in the spectrum, indicating the mixing of fusion products to the surface and a strong stellar wind.

It has a surface gravity of , typical for a giant star, but around 25 times lower than the Earth's and 700 times lower than the sun's. Its metallicity is about 30% lower than the sun's. Measurements by the Hipparcos satellite and other sources put Aldebaran around away. Asteroseismology has determined that it is about 16% more massive than the Sun, yet it shines with 518 times the Sun's luminosity due to the expanded radius.

This is an evolved G-type giant star with a stellar classification of G7 III. It is a red clump star, which means it is generating energy through helium fusion at its core. The star has an estimated 1.81 times the mass of the Sun and it has expanded to 11 times the Sun's radius. It is radiating 69 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,150 K.

The primary, designated component A, is an aging giant star with a stellar classification of G8III. It is 302 million years old with 3.3 times the mass of the Sun. With the supply of hydrogen at its core exhausted, the star has now expanded to 16 times the Sun's radius. It is a red clump giant on the horizontal branch, which indicates it is generating energy through the fusion of helium at its core.

The spectral class of FK Comae Berenices is G4 III, although it is considered unusual in having very broad absorption lines as well as some emission lines. The broadened spectral lines are due to rapid rotation. The rotation rate of FK Comae Berenices is unusually fast for a cool giant star. It is speculated that this is due to the merger of a contact binary pair of stars into a single star.

Based upon a stellar classification of F2 III, this matches an aging giant star that has exhausted the hydrogen at its core and is evolving away from the main sequence. It is a possible pulsating Delta Scuti variable, although there is some uncertainty about this classification. However, Kunzli and North (1998) found no variation. The star is 1.44 billion years old with 1.8 times the mass of the Sun and 3.2 times the Sun's radius.

Phi3 Ceti is a solitary, orange-hued star in the equatorial constellation of Cetus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.31. Based upon an annual parallax shift of 5.92 mas as seen from Earth, it is located roughly 550 light years from the Sun, give or take 30 light years. This is an evolved K-type giant star with a stellar classification of K5 III.

This is an evolved K-type star with a stellar classification of K0 II-III, displaying a luminosity class with mixed traits of a bright giant (II) and a giant star (III). With the supply of hydrogen at its core exhausted, the star has expanded to 16.8 times the radius of the Sun. It is radiating 152 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,942 K.

This is an aging giant star with a stellar classification of . The suffix notation indicates abnormally weak lines of carbyne. Having exhausted the hydrogen at its core, the star evolved away from the main sequence by expanding to 11 times the Sun's radius. The star is radiating 65.6 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,953 K. It is a suspected variable star of unknown type.

Alpha Lupi (α Lupi, α Lup) is a blue giant star, and the brightest star in the southern constellation of Lupus. According to the Bortle Dark-Sky Scale, its apparent visual magnitude of 2.3 makes it readily visible to the naked eye even from highly light-polluted locales. Based upon parallax measurements made during the Hipparcos mission, the star is around from the solar system. It is one of the nearest supernova candidates.

It is a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.345. The visible component is an evolved giant star with a stellar classification of . This is a mild barium star with the suffix notation above indicating associated abundance anomalies. The companion is a presumed white dwarf star that has already passed through its giant stage, during which time it enhanced the envelope of the companion with s-process elements.

The absolute magnitude is −0.55. The primary component of this system, component A, is an aging giant star with a stellar classification of G9III and a visual magnitude of 5.09. The secondary companion, designated component B, is a magnitude 6.94 star located at an angular separation of from the primary, along a position angle of 157°, as of 2016. It is an F-type main- sequence star with a class of F5V.

Delta Ophiuchi has a stellar classification of M0.5 III, making this a red giant star that has undergone expansion of its outer envelope after exhausting the supply of hydrogen at its core. It is currently on the asymptotic giant branch. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of Delta Ophiuchi, this yields a physical size of about 59 times the radius of the Sun.

Tau4 Serpentis, Latinized from τ4 Serpentis, is a M-type bright giant star in the constellation of Serpens, approximately 520 light-years from the Earth. It is classified as a semiregular late-type variable star, and its magnitude varies between +5.89 and +7.07 with a period of approximately 100 days. τ4 is unique among the stars with the Bayer designation τ Serpentis as being the only one with no HR catalog number.

The brighter member, component Aa, is an evolved K-type giant star with a stellar classification of K0 III. It is a red clump star that is generating energy by helium fusion at its core. The star has an estimated 2.36 times the mass of the Sun and has expanded to 8 times the Sun's radius. It is radiating 36 times the solar luminosity from its photosphere at an effective temperature of 4,853 K.

82 Cancri (Pi2 Cancri, π2 Cancri) is a solitary, orange-hued star in the zodiac constellation of Cancer. This is an evolved K-type giant star with a stellar classification of K1 III. With an apparent visual magnitude of +5.33, it is visible to the naked eye on a dark night. Based upon an annual parallax shift of 5.37 mas as seen from Earth, this star is located roughly 610 light years from the Sun.

It has a high peculiar velocity of and may be a runaway star. The stellar classification of this star is , showing the spectrum of an evolved K-type giant star with an overabundance of CN in the atmosphere. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of this star, this yields a physical size of about 77 times the radius of the Sun.

Alpha Sculptoris, Latinized from α Sculptoris, is the Bayer designation for a blue-white star in the southern constellation of Sculptor. It has an apparent visual magnitude of +4.30, which makes it the brightest star in this generally faint constellation. Parallax measurements collected during the Hipparcos mission provide a distance estimate for this star, placing it at roughly , with a 4% margin of error. Alpha Sculptoris is a B-type giant star.

Beta Sculptoris, Latinized from β Sculptoris, is a single, blue-white hued star in the southern constellation of Sculptor. It has an apparent visual magnitude of 4.37, which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 18.74 mas as seen from Earth, it is located 174 light years from the Sun. This is a B-type giant star with a stellar classification of B9.5IIIp(HgMnSi).

Kappa2 Sculptoris, Latinized from κ2 Sculptoris, is a solitary, orange-hued star in the southern constellation of Sculptor. It is faintly visible to the naked eye, with a combined apparent visual magnitude of +5.42. Based upon an annual parallax shift of 4.11 mas as measured from Earth, it is located approximately 800 light years from the Sun. This is an evolved K-type giant star with a stellar classification of K2 III.

MWC 349 is a resolved double star, with its components separated by 2.4 arc seconds. The primary, MWC 349A, is a B[e] star, where the B is the spectral type and the [e] denotes forbidden emission lines. Its spectrum lacks absorption features and is variable but has been classified as B0-1.5 with a supergiant luminosity class. The secondary, MWC 349B, is a giant star with a spectral type of B0III.

Such stars are termed ellipsoidal variables. Within a few million years, as the primary continues to evolve into a red giant star, the system may become a semi-detached binary with the Roche lobe becoming filled to overflowing. The mean apparent magnitude of +3.42 for this pair is bright enough to be readily seen with the naked eye. It forms the second brightest star or star system in this generally faint constellation, following Beta Trianguli.

Zeta Telescopii (ζ Telescopii) is the second-brightest star in the southern constellation of Telescopium. It is a solitary, orange-hued star that is visible to the naked eye with an apparent visual magnitude of +4.13. Based upon an annual parallax shift of 25.84 mas as seen from Earth, it is located around 127 light years from the Sun. This is a red clump giant star of spectral type K1 III-IV.

At that range, the visual magnitude of the star is diminished by an extinction factor of 0.24 due to interstellar dust. This is an evolved G-type giant star with a stellar classification of , where the suffix notation indicates an underabundance of iron in the spectrum. The measured angular diameter is . At the estimated distance of Pi Tauri, this yields a physical size of about 21 times the radius of the Sun.

This is a single-lined spectroscopic binary with an orbital period of 4.4 years and an eccentricity of 0.2. The visible component is an evolved K-type giant star with a stellar classification of K0/1 III. It is currently on the horizontal branch and thus is generating energy through helium fusion at its core. Delta Microscopii has nearly twice the mass of the Sun and has expanded to 11 times the Sun's radius.

HD 221246 or NGC 7686 1 is a star in open cluster NGC 7686, and it belongs to the northern constellation of Andromeda. With an apparent visual magnitude of 6.17, it can be viewed by the naked eye only under very favourable conditions. It has a spectral classification of K3III, meaning it is an evolved orange giant star. Parallax measurements place this star about 1,000 light years away from the solar system.

HD 221776 is a double star in the northern constellation of Andromeda. With an apparent visual magnitude of 6.18,, it is viewable by the naked eye user very favourable conditions. The most luminous component has a spectral classification K5III, meaning that it's an orange giant star that has evolved off the main sequence. An infrared excess has been detected around this star, indicating the star is associated with a cloud of dust particles.

In the past this star has been considered a member of the open cluster NGC 1252, but this now seems unlikely. This is an aging red giant star on the asymptotic giant branch with a stellar classification of C-N4IIIb:. It is one of the brightest carbon stars and has a type of C2 3.5. The star is classified as a semiregular variable of type SRb and has a periodicity of 158 days.

With a stellar classification of G6/8 III, Upsilon¹ Hydrae is an evolved G-type giant star. It has an estimated 3.3 times the mass of the Sun and has expanded to 14.7 times the Sun's radius. The star is about 270 million years old with a projected rotational velocity of just 2.11 km/s. It is radiating 162 times the Sun's luminosity from its photosphere at an effective temperature of 5,185 K.

UZ Pyxidis is a carbon star. These types of stars are known for having large amounts of carbon in their atmospheres, forming carbon compounds that make the star appear strikingly red. It was first recognised as having an unusual spectrum in 1893. Under the Morgan–Keenan classification of carbon stars, UZ Pyxidis' spectral type is C55; if it were a normal giant star, this would correspond to a spectral type of about K5.

The visible component is a K-type giant star with a stellar classification of K0.5 III. It is most likely (78% chance) on the red giant branch and is around 1.55 billion years old. As such, it has an estimated double the mass of the Sun and about 18 times the Sun's radius. The star is radiating about 123 times the Sun's luminosity from its photosphere at an effective temperature of 4,574 K.

RU Andromedae is a variable star in the constellation of Andromeda. It is classified as a semiregular variable pulsating giant star, and varies from an apparent visual magnitude of 14.5 at minimum brightness to a magnitude of 9.9 at maximum brightness, with a period of approximately 238.3 days.RU And, database entry, Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.), N. N. Samus, O. V. Durlevich, et al., CDS ID II/250 Accessed on line 2009-06-30.

RV Andromedae is a variable star in the constellation of Andromeda. It is classified as a semiregular variable pulsating giant star, and varies from an apparent visual magnitude of 11.5 at minimum brightness to a magnitude of 9.0 at maximum brightness, with a period of approximately 168.9 days.RV And, database entry, Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.), N. N. Samus, O. V. Durlevich, et al., CDS ID II/250 Accessed on line 2009-06-30.

Based upon their motion through space, this system made its perihelion passage some 858,000 years ago when it came within of the Sun. It is currently moving away with a radial velocity of 48 km/s. The primary component is K-type giant star with a stellar classification of K0 III. It has a derived luminosity of around 53 times that of the Sun, 1.74 times the Sun's mass and is about 5.27 billion years old.

The spectral classification of 14 Persei is as a G0 yellow supergiant, but in other respects it appears to be a giant star. The class has been given as or , where the abundance suffixes indicate stronger Calcium lines than expected for its class, or weaker hydrocarbons. Other analyses of the spectrum give a class of G0Ib. Stellar models of 14 Persei yield an estimated mass four times that of the Sun and an age of 162 million years.

110 Virginis is a star in the zodiac constellation Virgo, located 195 light- years away from the Sun. It is visible to the naked eye as an orange-hued star with an apparent visual magnitude of 4.40. The star is moving closer to the Earth with a heliocentric radial velocity of −16 km/s. The stellar classification of 110 Virginis is , indicating that this is an evolved giant star with a mild underabundance of iron in its spectrum.

Delta Crateris (δ Crt, δ Crateris; traditional name: Labrum) is a solitary star in the southern constellation of Crater. With an apparent visual magnitude of 3.56, it is the brightest star in this rather dim constellation. It has an annual parallax shift of 17.56 mas as measured from Earth, indicating Delta Crateris lies at a distance of 163 ± 4 light years from the Sun. This is an evolved orange-hued giant star belonging to the spectral class K0 III.

Based upon parallax measurements, the star is located approximately 830 light years away from the Sun. It is moving closer to the Earth with a heliocentric radial velocity of −16 km/s. This is an aging bright giant star with a stellar classification of K2.5IIb, having exhausted the supply of hydrogen at its core and expanded to 100 times the radius of the Sun. It is 64 million years old with 6.2 times the Sun's mass.

63 Ophiuchi is an O-type giant star in the constellation Sagittarius, despite its name. During a 2009 survey for companions of massive stars, it was observed using speckle interferometry but no companion was found. Uncertain negative parallax measurements of –0.77 ± 0.40 mas suggest that this extremely luminous star may be located about 4000 light-years away. An estimate of the distance based on the strength of the Ca II line yields a more modest value of .

Psi Leonis is an evolved red giant star with a stellar classification of M2 IIIab. It shines with a luminosity over 900 times that of the Sun from a relatively cool outer atmosphere that has an effective temperature of 3,756. It is a suspected variable star with a measured brightness variation of 0m.018. Psi Leonis has a magnitude 11.63 visual companion at an angular separation of 281.60 arcseconds along a position angle of 139°, as of 2000.

Omicron¹ Eridani is an evolved F-type giant star with a stellar classification of F0 III. It is a Delta Scuti variable star that undergoes non-radial pulsations, with a variation of just 0.03 magnitude over a period of 0.0747 days. The star is spinning rapidly with a projected rotational velocity of 108.1 km/s and a rotation period of less than around 1.9 days. This is creating an equatorial bulge that is 11% wider than the polar radius.

The stellar classification of A1 III suggests this is an evolved giant star, although Malagnini and Morossi (1990) rated it as an A2 IV subgiant star. It has an estimated age of 260 million years. This star does not show an excess emission of infrared radiation that might otherwise suggest the presence of a debris disk. It has about 3.5 times the Sun's mass and has expanded to almost seven times the radius of the Sun.

A yellow giant is a luminous giant star of low or intermediate mass (roughly 0.5–12 solar masses (M)) in a late phase of its stellar evolution. The outer atmosphere is inflated and tenuous, making the radius large and the surface temperature as low as 5,200-7500 K. The appearance of the yellow giant is from white to yellow, including the spectral types F and G. About 10.6 percent of all giant stars are yellow giants.

A diagonal burr - Giant Star puzzle (manufactured by Gaya Games) Though most burr puzzle pieces are made with square notches, some are made with diagonal notches. Diagonal burr pieces are square sticks with V-shaped notches, cut at an angle of 45° off the stick's Face. These puzzles are often called "Stars", as it is customary to also cut the sticks' edges at an angle of 45°, for aesthetic reasons, giving the assembled puzzle a Star-like shape.

This name was later connected by Allen with 46 Leonis Minoris—an error perpetuated by subsequent astronomers. The original "Praecipua", 37 Leonis Minoris, has an apparent magnitude of 4.69, but is a distant yellow supergiant of spectral type G2.5IIa and absolute magnitude of −1.84, around distant. Leo Minor as seen by the naked eye Beta Leonis Minoris is a binary star system. The primary is a giant star of spectral class G8 and apparent magnitude of 4.4.

HD 107914 is a binary star in the constellation Centaurus, with an estimated distance of from the Solar System. The primary has a stellar classification of A7-8 III, making it a giant star. Measurement of the proper motion of this system show that it has a low transverse velocity relative to the Sun. For this reason, it has been compared to the hypothetical "Nemesis" star since it may pass through the Oort cloud in the future.

This is a set of stars centered on Wolf 630 that are moving nearly in parallel and have an age of around billion years. They may be former members of a dissolved open cluster. At an age of about 2.21 billion years, Phi1 Ceti is an evolved red clump giant star with a stellar classification of K0 III. It is presently on the horizontal branch and is generating energy through the nuclear fusion of helium at its core.

Consequently, the Chinese name for ν Ceti itself is "the Seventh Star of Circular Celestial Granary", . AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日 The primary, designated component A, forms a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.27. The visible component is a G-type giant star, currently on the horizontal branch, with a stellar classification of G8III.

With an age of 350 million years, this is an A-type star of stellar classification A2 IIIs, where the luminosity class of III typically indicates an evolved giant star and the 's' means the spectrum displays sharp absorption lines. It is a candidate Am star, meaning there are some chemical peculiarities. The measured angular size is . At the estimated distance of Pi Draconis, this yields a physical size of about 3.2 times the radius of the Sun.

14 Andromedae b (abbreviated 14 And b), formally named Spe , is an extrasolar planet approximately 249 light years away in the constellation of Andromeda. The 186-day period planet orbits about 83% the Earth-Sun distance from the giant star 14 Andromedae. It has a minimum mass 4.8 times the mass of Jupiter. The planet orbits with an eccentricity of 0.0094, which means the orbital distance over the course of its revolution varies by only 0.02 AU.

Zeta Apodis, Latinized from ζ Apodis, is the Bayer designation for a star in the southern constellation of Apus. It has an apparent visual magnitude of +4.78, which is bright enough to allow it to be seen with the naked eye. The distance to this star is known from parallax measurements to be around . The spectrum of Zeta Apodis matches a stellar classification of K2 III, with the luminosity class of III indicating it is an evolved giant star.

The companion star that was hit is suspected to be a red giant star. This detection of the UV signal represents the first time the collision event of a supernova shockwave upon a companion star has been detected. The supernova was discovered by the Intermediate Palomar Transient Factory (iPTF), a successor to the earlier Palomar Transient Factory, and based at the Palomar Observatory in California. The data was processed by collaborators in Europe, that lead to the supernova discovery.

At this distance, the brightness of the system is diminished by 0.065 in visual magnitude from extinction caused by interstellar gas and dust. This is a spectroscopic binary system where the presence of an orbiting companion is revealed by shifts in the spectral lines caused by the Doppler effect. The primary component is a giant star with a stellar classification of G8 III. The secondary is following a circular orbit with a period of 205.2 days.

The system is moving closer to the Earth with a heliocentric radial velocity of –23 km/s. The primary component of this system is a magnitude 5.31 K-type giant star or bright giant with a stellar classification of K1. The star is radiating 155 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,660 K. Orbiting at an angular separation of 3.25 arcseconds is a magnitude 8.76 companion star.

This is an evolved K-type giant star with a stellar classification of . The 'Ba0.4' suffix notation indicates this is a barium star, which means that the stellar atmosphere has been enhanced by s-process elements most likely provided by what is now an orbiting white dwarf companion. The giant component has times the radius of the Sun. It is radiating 1,626 times the Sun's luminosity from its enlarged photosphere at an effective temperature of about 3,917 K.

It is moving closer to the Earth with a heliocentric radial velocity of –5 km/s. The stellar classification of this star is B8 II-III, with the luminosity class of II-III suggesting that the spectrum displays elements of both a giant star and a bright giant. It is a chemically peculiar star of the Mercury-Manganese type (CP3). This is a probable Alpha2 Canum Venaticorum variable that ranges in visual magnitude from 5.06 down to 5.16.

It is moving closer to the Earth with a heliocentric radial velocity of −30 km/s. The motion of the star over time suggests some displacement, which may indicate it is a close binary system. This is an aging giant star with a stellar classification of K5 III, which indicates it has exhausted the supply of hydrogen at its core and expanded off the main sequence. The measured angular diameter of this star, after correcting for limb darkening, is .

At this distance, the brightness of the star is diminished from extinction caused by interstellar gas and dust. The spectrum of 27 Aquilae fits a stellar classification of B9 III, with the luminosity class of III typically indicating this is an evolved giant star. As it lies within the field of view of the CoRoT satellite, close observation have been made of its luminosity. The star shows a multiperiodic variability with at least six pulsation frequencies discovered.

62 Aquilae is a single star located about 427 light years away from the Sun in the equatorial constellation of Aquila. 62 Aquilae is its Flamsteed designation. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.67. This is an aging giant star with a stellar classification of K4 III, having exhausted the supply of hydrogen at its core and expanded to 23 times the girth of the Sun.

The stellar classification for this star is A2IIIvs, matching an A-type giant star with narrow (sharp) absorption lines. Abt and Levy (1985) classed it as a kA2hA6mA6 star, which indicates the spectrum has the calcium K line of an A2 star, the hydrogen lines of an A6 star, and the metal lines of an A6 star. It is around 450 million years old and is spinning with a projected rotational velocity of 84 km/s.

This object is an aging giant star with a stellar classification of G5 III, most likely (96% chance) on the horizontal branch. Having exhausted the supply of hydrogen at its core, the star has expanded to 35 times the Sun's radius. It is around 219 million years old with 3.7 times the mass of the Sun. The star is radiating 533 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,665 K.

At that distance, the brightness of the star is diminished by 0.21 in magnitude from extinction caused by interstellar gas and dust. This is a red giant star with a stellar classification of M0 III. It is a semi-regular variable with periods of 32 and 275 days; the brightness of the star changes by an amplitude of 0.14 in magnitude during those intervals. The measured angular diameter of this star, after correction for limb darkening, is .

This object is an evolved giant star with a stellar classification of K1 III, most likely (82% chance) on the horizontal branch. It is around 470 million years old with a projected rotational velocity of 3.4 km/s. The star has over three times the mass of the Sun and has expanded to 11 times the Sun's radius. It is radiating 70 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,980 K.

14 Andromedae, abbreviated 14 And, also named Veritate , is a single, orange- hued giant star situated approximately 247 light-years away in the northern constellation of Andromeda. It is dimly visible to the naked eye with an apparent visual magnitude of 5.22. The star is moving closer to the Earth with a heliocentric radial velocity of −60 km/s. In 2008 an extrasolar planet (designated 14 Andromedae b, later named Spe) was discovered to be orbiting the star.

It is moving closer to the Sun with a heliocentric radial velocity of −11.5 km/s. With an estimated age of years, this is an aging red clump giant star with a stellar classification of K0 III, indicating it is generating energy by helium fusion at its core. The spectrum displays "slightly strong" absorption lines of cyanogen (CN). It has 2.07 times the mass of the Sun and has expanded to 11 times the Sun's radius.

It is located approximately 111.6 light years away from the Sun based on parallax. The star is drifting further from the Earth with a heliocentric radial velocity of +38 km/s. This object has a stellar classification of F5III-IV, matching an F-type star with a luminosity class displaying mixed traits of a subgiant and a giant star. It is 1.2 billion years old with 1.7 times the mass of the Sun and 3.2 times the Sun's radius.

7 Boötis is a single star in the northern constellation of Boötes, located 590 light years away from the Sun. It is barely visible to the naked eye as a dim, yellow-hued star with an apparent visual magnitude of 5.71. 7 Boötis is moving closer to the Earth with a heliocentric radial velocity of −11 km/s. This is an evolved giant star with a stellar classification of G5 III, currently at the end of the Hertzsprung gap.

11 Boötis is a star in the northern constellation of Boötes, located 333 light years away from the Sun. It is near the lower limit of visibility to the naked eye, appearing as a dim, white-hued star with an apparent visual magnitude of 6.23. This body is moving closer to the Earth with a heliocentric radial velocity of −24 km/s. It has a stellar classification of A7 III, matching an evolved A-type giant star.

Tau Cassiopeiae (τ Cassiopeiae) is a solitary, orange hued star in the northern constellation of Cassiopeia. It is bright enough to be seen with the naked eye, having an apparent visual magnitude of +4.86. Based upon an annual parallax shift of 18.75 mas as seen from Earth, this system is located about 174 light years from the Sun. The spectrum of this star indicates it is an evolved, K-type giant star with a stellar classification of K1 IIIa.

This is a red clump giant star with a stellar classification of K2 IIIb. It is around 5.4 billion years old with a projected rotational velocity that is too small to be measured. The star has expanded to about 15 times the radius of the Sun and shines with 79 times the solar luminosity from its outer atmosphere at an effective temperature of 4,498 K. Omicron2 Orionis is most likely a member of the Milky Way's thin disk population.

This is an aging giant star with a stellar classification of K1.5III-IIIb CN-1, where the suffix notation indicates an underabundance of cyanogen in the spectrum. Having exhausted the supply of hydrogen at its core, this star cooled and expanded off the main sequence. At present it has 25 times the radius of the Sun. HD 40657 is a suspected variable star with a brightness that has been measured ranging from magnitude 4.54 down to 4.58.

The star has a peculiar velocity of relative to its neighbors, and may be a runaway star. This object is a bright giant star with a stellar classification of K2-IIb. It is a suspected variable star of unknown type with a brightness that has been measured varying from 4.73 down to 4.78. The star is about 61 million years old with 6.4 times the mass of the Sun and is spinning with a projected rotational velocity of 3.5.

This system has an orbital period of 118.16 years with an eccentricity of 0.030 and a semimajor axis of . The primary member, designated component A, is a magnitude 5.32 giant star with a stellar classification of K0 III. It is a red clump giant, which means it is on the horizontal branch and is generating energy through helium fusion at its core. This star has 1.44 billion years old with 2.32 times the mass of the Sun.

This is an aging giant star with a stellar classification of , having exhausted the supply of hydrogen at its core and expanded to 22 times the Sun's radius. The suffix notation indicates it displays an overabundance of calcium in its spectrum. It is a red clump giant, which means it is on the horizontal branch and is generating energy through helium fusion at its core. The star is about 1.2 billion years old with 2.3 times the Sun's mass.

Based upon the spectrum of this star, it has a stellar classification of K0 III. This indicates this is an evolved K-type giant star that has exhausted the hydrogen at its core and has left the main sequence. This is a red clump star, which means it is now generating energy through helium fusion at its core. It has 10% of the mass of the Sun and has expanded to over ten times the Sun's radius.

HD 115004 will make its closest approach in about 1.7 million years at a separation of around . This is an evolved giant star, most likely (97% chance) on the horizontal branch, with a stellar classification of . The suffix notation indicates a mild overabundance of the CN molecule in the stellar atmosphere. It has an estimated 3.2 times the mass of the Sun and, at the age of 440 million years, has expanded to 23 times the Sun's radius.

At the age of 1.1 billion years, this is an evolved red giant star with a stellar classification of M3- IIIa. It is a slow irregular variable of type Lb, with a brightness that ranges between magnitudes 4.73 and 4.85. The star has 2.2 times the mass of the Sun and has expanded to 117 times the Sun's radius. It is radiating 2,387 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,529 K.

There has been some uncertainty as to the classification of this stage. Houk (1979) lists a stellar class of B8 Ib/II for HD 161840, which corresponds to a B-type bright giant/lesser supergiant mix. Multiple studies still use an older classification of B8 V, suggesting instead this is a B-type main-sequence star. Garrison and Gray (1994) assigned it a class of B8 III-IV, which would put it on the subgiant/giant star track.

The star made its closest approach to the Sun some 8.7 million years ago at a separation of around . Roughly 40 million years old, this is an evolved K-type giant star with a stellar classification of . The suffix notation indicates overabundances of calcium and the cyanide molecule have been found in the spectrum of the stellar atmosphere. The star has 7.4 times the mass of the Sun and has expanded to 28 times the Sun's radius.

At its present distance, the visual magnitude of the system is diminished by an extinction factor of due to interstellar dust. This system's binary nature was discovered in 1878 by an amateur astronomer, S. W. Burnham. It has an orbital period of roughly 850 years, a semimajor axis of 1.2 arc seconds, and an eccentricity of 0.47. The primary, component A, is an evolved, magnitude 3.83 G-type giant star with a stellar classification of G7 IIIa.

The primary component is an evolved giant star with a stellar classification of K3 III. It has expanded to 19 times the radius of the Sun, from which it is radiating 120 times the Sun's luminosity. This energy is being emitted into outer space from the outer atmosphere at an effective temperature of 4,406 K, giving it the cool orange glow of a K-type star. At an angular separation of 0.53 arcseconds is a magnitude 8.50 companion.

Xi1 Capricorni, Latinized from ξ1 Capricorni, is an orange-hued star in the constellation Capricornus. With an apparent visual magnitude of +6.34, it is near the lower limit of brightness for stars that can be seen with the naked eye. Based upon an annual parallax shift of 6.95 mas as seen from Earth, this system is located roughly 470 light years from the Sun. It is an evolved K-type giant star with a stellar classification of K0 III.

The binary nature of this system was first detected as an ultraviolet excess in 1996. No radial velocity variation has been detected so it must be a wide system with an orbital period of up to 21 years. The estimated semimajor axis of their orbit is . The pair were not resolved using the Hubble Space Telescope WFPC2 instrument. The primary is an evolved bright giant star with a yellow-white hue and a stellar classification of F8II.

The object is drifting further away with a radial velocity of +63 km/s, having come to within some 1.8 million years ago. This is an aging giant star with a stellar classification of K3 III, which means it is no longer undergoing core hydrogen fusion. It has expanded to 30 times the Sun's radius and is radiating 279 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,289 K.

The brighter component of this system is an evolved, yellow-hued, G-type giant star with a stellar classification of G6/8 III. It is a semiregular variable that ranges between apparent magnitudes 3.99 and 4.2, located 325 light-years from Earth. Delta1 Gruis has around 3 times the mass and 135 times the diameter of the Sun. The fainter companion is a magnitude 12.8 star at an angular separation of 5.6 arc seconds, as of 2008.

According to the main author of the paper in Nature which announced the discovery of the two planets, Stephane Charpinet, the two planets "probably plunged deep into the star's envelope during the red giant phase, but survived." However, this is not the first sighting of planets orbiting a post-red giant star - numerous pulsar planets have been observed, including one that orbits closer to its host star, and consequently in a shorter time than, any other planet.

42 Herculis is a single star located around 450 light years away from the Sun in the northern constellation of Hercules. It is visible to the naked eye as a faint, red-hued star with an apparent visual magnitude of 4.86. The star is moving closer to the Earth with a heliocentric radial velocity of −56 km/s. This is an aging red giant star on the asymptotic giant branch with a stellar classification of M2.5III.

This is an aging red giant star on the asymptotic giant branch with a stellar classification of M3 III. It is a semiregular variable with an amplitude of 0.14 in the B-band and pulsation periods of 22.9 and 24.0 days. Having exhausted the hydrogen at its core, the star has expanded to 86 times the Sun's radius. It is radiating 1,202 times the Sun's luminosity from its swollen photosphere at an effective temperature of 3,535 K.

32 Ophiuchi is a single star located 410 light years away from the Sun in the constellation Hercules. It is visible to the naked eye as a dim, red-hued star with an apparent visual magnitude of 4.97. This is an aging red giant star on the asymptotic giant branch with a stellar classification of M3−III. Having exhausted the supply of hydrogen at its core it has expanded to 60 times the girth of the Sun.

The star has a relatively high proper motion, traversing the celestial sphere at the rate of 0.195 arc seconds per annum. This is an aging giant star with a stellar classification of K4.5 III. It displays an enhanced abundance of elements generated through the alpha process, and, in particular, has a strong enhancement of silicon. 29 Herculis is a suspected variable star of unknown type, and has been measured ranging in visual magnitude from 4.82 down to 4.85.

HD 35984 is star in the northern constellation Auriga. It has an apparent magnitude of 6.20, which, according to the Bortle scale, indicates it is faintly visible to the naked eye from dark rural skies. Parallax measurements by the Hipparcos satellite indicates it lies at a distance of roughly 290 light years away. A stellar classification of F6III suggests that this is an evolved giant star that has consumed the supply of hydrogen at its core.

Gaga got up from her seat and proceeded to perform the song in the middle of the stage. She wore a silvery leotard with a giant star on her shoulder and tassels. As the song progressed to the intermediate verse, the violinist played a hoe-down version of the music and Gaga danced around frantically over the stage. The performance ended with Gaga staring towards the audience while revealing an open zipper, patched over her left eye.

It forms a triangle with the fainter φ1 Hydrae and φ2 Hydrae, between μ Hydrae and ν Hydrae. This is a single-lined spectroscopic binary star system with an orbital period of about 1,200 days and an eccentricity of 0.1. The primary, component A, is an evolved G-type giant star with a stellar classification of G8 III. It is a red clump star, which means it is generating energy through the fusion of helium at its core.

R Cygni light curve, showing the period-doubling R Cygni is a variable star of the Mira type in the constellation Cygnus, less than 4' from θ Cygni. This is a red giant star on the asymptotic giant branch located around 2,200 light years away. It is an S-type star ranging between spectral types S2.5,9e to S6,9e(Tc). Stars at this mass range and evolutionary stage are pulsationally unstable, displaying a variation in their light output.

18 Delphini b (abbreviated 18 Del b), formally named Arion , is an extrasolar planet approximately 249 light-years away in the constellation of Delphinus. The 993-day period planet orbits the yellow giant star 18 Delphini. A very massive and dense planet with a minimum mass of it was discovered on February 19, 2008 by Sato. In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars.

This is an evolved giant star with a stellar classification of K2.5 III. It is a red clump giant, meaning it is fusing helium in its core after passing through the red giant branch. The star is 3.2 billion years old with 1.38 times the mass of the Sun and has expanded to 27.7 times the Sun's radius. It is radiating 204 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,352 K.

Curious spiral around red giant star R Sculptoris. No stars brighter than 3rd magnitude are located in Sculptor. This is explained by the fact that Sculptor contains the south galactic pole where stellar density is very low. Overall, there are 56 stars within the constellation's borders brighter than or equal to apparent magnitude 6.5. The brightest star is Alpha Sculptoris, an SX Arietis-type variable star with a spectral type B7IIIp and an apparent magnitude of 4.3.

Delta Muscae, Latinized from δ Muscae, often catalogued as HD 112985, is a spectroscopic binary star system and the closest to the Earth in the southern hemisphere constellation of Musca (the Fly) at a distance of approximately 27.8 parsecs (91.0 light years). The main star is classified as a giant star with an orange tint. It is one of the stars given a Bayer designation by astronomer Johann Bayer. It was recorded in Bayer's 1603 publication Uranometria.

Delta Muscae has a listed spectral type of K2III. The K2 portion of this designation specifies that Delta Muscae A is a class K2 star, meaning the light it emits is orange in color. The main star burns at a temperature cooler than the Sun, which is a G2 star. The second part of the classification, III, specifies that Delta Muscae is a giant star which has already left the main sequence of star life like the Sun.

Map showing location of NGC 7510 (Roberto Mura) NGC 7510 is an open cluster of stars located around 11,400 light years away in the constellation Cepheus, near the border with Cassiopeia. At this distance, the light from the cluster has undergone extinction from interstellar gas and dust equal to = magnitude in the UBV photometric system. Its brightest member is a giant star with a stellar classification of B1.5 III. This cluster forms part of the Perseus Spiral Arm.

This is an evolved K-type giant star with a stellar classification of K1 III. It is a red clump giant, which indicates it is on the horizontal branch and is generating energy through helium fusion at its core. The star is 4.1 billion years old with 1.34 times the mass of the Sun and 13 times the Sun's radius. It is radiating 69 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,665 K.

It is moving further from the Sun with a heliocentric radial velocity of 9.5 km/s. This is an evolved K-type giant star with a stellar classification of K0 III-IIIb. At the age of 1.39 billion years, it has become a red clump giant, indicating that it is generating energy through helium fusion at its core. The star has around double the mass of the Sun and has expanded to 10 times the Sun's radius.

This is an evolved K-type giant star with a stellar classification of K0 III. It is a red clump star that is generating energy via helium fusion at its core. At the estimated age of 1.65 billion years, Omega Persei has double times the mass of the Sun and has expanded to about 19 times the Sun's radius. It is radiating 144.5 times the Sun's luminosity from its photosphere at an effective temperature of 4,586 K.

NGC 2423-3b is an extrasolar planet approximately 2498 light-years away in the constellation of Puppis. The planet was announced in 2007 to be orbiting the red giant star NGC 2423-3 (which in turn is part of the NGC 2423 open cluster). The planet has a mass at least 10.6 times that of Jupiter. Only the minimum mass is known since the orbital inclination is not known, so it may instead be a brown dwarf.

This is a giant star of type K with a stellar classification of K3III, indicating that it has exhausted the hydrogen at its core and evolved away from the main sequence. It is about two billion years old with 1.5 times the mass of the Sun and has expanded to 28 times the Sun's radius. The star is shining with around 302 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,294 K.

The star is moving closer to the Sun with a radial velocity of −19 km/s. This is a B-type giant star with a stellar classification of B6 III. It has 4.6 times the Sun's radius and is radiating 676 times the solar luminosity from its photosphere at an effective temperature of 13,614 K. The star may be slightly variable, occasionally brightening to magnitude 3.95. It is spinning with a projected rotational velocity of 52 km/s.

Consequently, the Chinese name for ι Ceti itself is (, .) 香港太空館 - 研究資源 - 亮星中英對照表 , Hong Kong Space Museum. Accessed on line November 23, 2010. This is an MK-standard star with a stellar classification of K1.5 III, indicating that it is an evolved K-type giant star. However, Houk and Swift (1999) list a classification of K1 II, which would indicate this is a bright giant.

It is drifting closer with a radial velocity of −19 km/s. This is an evolved G-type giant star with a stellar classification of G8 III. At the estimated age of 1.5 billion years, is a red clump giant on the horizontal branch, which indicates it is generating energy through helium fusion at its core. The star has about 1.76 times the mass of the Sun and has expanded to 11 times the Sun's radius.

The system appears as a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.38. The a sin i value for the primary is , where a is the semimajor axis and i is the (unknown) orbital inclination. This value provides a lower bound on the actual semimajor axis for the orbit. The primary component is an aging giant star with a stellar classification of , indicating a mild barium star with an underabundance of iron.

Lacking the strength to engage the Lugovalians, the Regeinlandics decide to seal off the starlane to the LMC. Yuri leads an attack on their fleet and manages to cripple their flagship. Nia boards the flagship and is mortally wounded while attempting to kill the Lugovalian commander. Meanwhile, the Regeinlandics deploy a prototype "exalaser" and cause a nearby red giant star to go supernova, wiping out much of both fleets and enveloping the Void Gate that leads to the LMC.

Based upon parallax measurements, Beta Pegasi is located about from the Sun. It is unusual among bright stars in having a relatively cool surface temperature compared to stars like the Sun. This star has a stellar classification of M2.3 II–III, which indicates the spectrum has characteristics partway between a bright giant and a giant star. It has expanded until it is some 95 times as large, and has a total luminosity of 1,500 times that of the Sun.

This is a spectroscopic binary star system with components that orbit each other every 3848.8 days (10.5 years). The combined stellar classification of the system is K0.5 IIIb, which matches the spectrum of a normal luminosity giant star. It has an apparent visual magnitude of 2.4, so it is somewhat outshined by its first magnitude neighbors Achernar (α Eridani) and Fomalhaut (α Piscis Australis). Based upon parallax measurements, this system is at a distance of about from the Earth.

It is an evolved giant star of the spectral type K2 III. It has double the mass of the Sun and has expanded to 27 times the Sun's radius. Tau Geminorum is radiating 224 as much radiation as the Sun from its expanded outer atmosphere at an effective temperature of 4,528 K, giving it the characteristic orange-hued glow of a K-type star. It appears to be rotating slowly with a projected rotational velocity of .

Tau Geminorum, Latinized from τ Geminorum, is a star in the northern zodiac constellation of Gemini. It has the apparent visual magnitude of +4.42, making it visible to the naked eye under suitably good seeing conditions. This star is close enough to the Earth that its distance can be measured using the parallax technique, which yields a value of roughly . Artist's illustration of the giant star Tau Geminorum (left) and its brown dwarf companion—the dark disk at right.

The visible component is an orange-hued giant star with a stellar classification of K1 III, having exhausted the hydrogen at its core and evolved away from the main sequence. It has an estimated 1.4 times the mass of the Sun and has expanded to 13 times the Sun's radius. At the age of 2.6 billion years, this star is radiating 96 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,660 K.

However, Cowley et al. (1969) gave it a class of F0 III, which would suggest it is instead an evolved giant star. The spectrum displays a higher than solar metallicity – a term indicating the abundance of elements other than hydrogen and helium compared to the Sun. The star is spinning with a projected rotational velocity of 50 km/s and is radiating 319 times the Sun's luminosity from its photosphere at an effective temperature of 7,623 K.

Mu1 Cancri, Latinized from μ1 Cancri, is an evolved red giant star in the zodiac constellation of Cancer. Parallax measurements made by the Hipparcos spacecraft put it about 740 light years (230 parsecs) from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.28. The name Mu1 comes from the Bayer naming system: the "1" in the name is because (from Earth) it appears to be close to 10 Cancri (Mu2 Cancri).

Upsilon1 Cancri, Latinized from υ1 Cancri, is the Bayer designation for a solitary, yellow-white hued star in the constellation Cancer. It is faintly visible with the naked eye, having an apparent visual magnitude of +5.7. Based upon an annual parallax shift of 13.05 mas as seen from Earth, this system is roughly 250 light years from the Sun. This object has a stellar classification of F0 IIIn, indicating it is an F-type giant star.

Upsilon2 Cancri (υ2 Cancri) is a faint, yellow-hued star in the zodiac constellation of Cancer. It is near the lower brightness limit of stars that can be viewed with the naked eye, having an apparent visual magnitude of +6.35. Based upon an annual parallax shift of 5.1325 mas as seen from our orbit, this system is roughly 635 light years away. This is an evolved G-type giant star with a stellar classification of G9 III.

17 Camelopardalis is a single star in the northern circumpolar constellation of Camelopardalis, located roughly 960 light years away from the Sun. It is visible to the naked eye as a faint, red-hued star with an apparent visual magnitude of 5.44. This object is moving closer to the Earth with a heliocentric radial velocity of −20 km/s. This is an aging red giant star, currently on the asymptotic giant branch, with a stellar classification of M1IIIa.

This is an aging giant star with a stellar classification of K1-III. After exhausting the supply of hydrogen at its core, the star cooled and expanded until currently it has 12 times the girth of the Sun. It is a red clump giant, which indicates it is presently on the horizontal branch and is generating energy through core helium fusion. The star is about 2.8 billion years old with 1.5 times the mass of the Sun.

Gamma Eridani (γ Eridani, abbreviated Gamma Eri, γ Eri), formally named Zaurak , is a variable star in the constellation of Eridanus. It is visible to the naked eye with an apparent visual magnitude that varies around 2.9, and lies at a distance of about 203 light years from the Sun, as determined by the Hipparcos astrometry satellite. This is an evolved red giant star that is currently on the asymptotic giant branch of the Hertzsprung–Russell diagram.

This relies on distance and luminosity estimates lower than most observations. The star would be an unusually large and bright giant star for the given mass, possibly as the result of very high mass loss. To match the observed eclipse and orbital data, the secondary is a fairly normal B main sequence star of about embedded in a thick disc seen nearly edge on. The orbit itself is now fairly well determined, inclined at over 87 degrees to Earth.

HR 8442 is a spectroscopic binary star in the constellation Cepheus. The primary is a G type giant star while the secondary's spectral type is unknown. The spectroscopic binary nature of the star was first noticed by Jose Renan de Medeiros and Michel Mayor using radial velocity measurements from the Coravel spectrometer at Haute-Provence Observatory. Roger griffin then placed the star on his observing program at Cambridge Observatory leading to an orbital solution being published in 2015.

At the age of around 686 million years, Nu Telescopii shows the spectral characteristics of an evolving A-type star with a stellar classification of A7 III–IV. Here, the luminosity class of III–IV indicates mixed traits of a subgiant and a giant star. It has about 1.85 times the mass of the Sun and 2.1 times the Sun's radius. Based upon its motion through space, it is a candidate for membership in the IC 2391 supercluster.

Xi Telescopii, Latinized from ξ Telescopii, is a solitary star in the southern constellation of Telescopium. It is visible to the naked eye, with an apparent visual magnitude of +4.95. Based upon an annual parallax shift of 3.02 mas as measured from Earth, it is located approximately 1,100 light years from the Sun. This is an evolved star with a stellar classification of K5 III or M1 IIab, indicating it is a giant or bright giant star.

The X-ray emission of Upsilon Andromedae A is low for a star of its spectral class. This means that the star may be moving, or move soon, out of the main sequence and expand its radius to become a red giant star. This is consistent with the upper limits on the age of this star. Upsilon Andromedae A was ranked 21st in the list of top 100 target stars for NASA's cancelled Terrestrial Planet Finder mission.

Alpha Trianguli Australis is a bright giant star with an apparent magnitude of +1.91. Based upon parallax measurements, this star is located roughly distant from the Earth. The estimated age of the star is 48 million years old; sufficiently old for a massive star to evolve away from the main sequence and expand into a giant. It has a mass roughly seven times the mass of the Sun, but is emitting about 5,500 times the Sun's luminosity.

According to the main author of the paper in Nature which announced the discovery of the two planets, Stephane Charpinet, the two planets "probably plunged deep into the star's envelope during the red giant phase, but survived." However, this is not the first sighting of planets orbiting a post-red giant star – numerous pulsar planets have been observed, but no planet has been found with such a short period around any star, whether or not on the main sequence.

Most studies categorized this as a K-type giant star with a stellar classification of K3 III. However, the results of a study published in 2003 list it with a classification of K3 Iab:, which would instead suggest it is a supergiant star. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of this star, this yields a physical size of about 27 times the radius of the Sun.

A stellar classification of K1 III reveals that this is a giant star, having expanded to an estimated 12 times the Sun's radius. This means it has exhausted the hydrogen in its core and evolved away from the main sequence. The abundance of elements other than hydrogen and helium in this star, what astronomers term the star's metallicity, is lower than in the Sun. Gamma² Sagittarii has an effective temperature of 4,760 K, compared to 5,778 K for the Sun.

Delta Volantis (δ Vol, δ Volantis) is a solitary star in the southern constellation Volans. It has an apparent visual magnitude of +3.97, which is bright enough to be seen with the naked eye. Based upon parallax measurements, is approximately 740 light years from the Sun. This is an F-type bright giant star with a stellar classification of F6 II. It has an estimated radius 24 times that of the Sun, and shines with more than a thousand times the Sun's luminosity.

It is classified a blue-white B-type giant star and has an apparent magnitude of +4.35. (The individual components are classified as B6IV and B8.) The binary system has an orbital period of 14.1683 days. The binary's companion, Epsilon Volantis B, is 6.05 arcseconds away and has an apparent magnitude of +8.1. It too is a spectroscopic binary, consisting of two A-type main sequence stars with stellar classifications of A2 V and an orbital period of "a few days".

The brightest component, κ1 Volantis, is a blue-white B-type star with a stellar classification showing characteristics of a both a subgiant and giant star. It has an unseen companion, and the pair form a single-lined spectroscopic binary. Separated from κ1 Volantis by 65 arcseconds, κ2 Volantis is a white subgiant star that falls between a B-type and A-type classification. The system's fourth component, κ Volantis C, is a magnitude +8.5 star 37.7 arcseconds away from κ2 Volantis.

109 Virginis is a single, white-hued star in the zodiac constellation of Virgo, located some 134.5 light years away from the Sun. It is the seventh- brightest member of this constellation, having an apparent visual magnitude of +3.72. This is an A-type main-sequence star with a stellar classification of A0 V, and is a suspected chemically peculiar star. However, Abt and Morrell (1995) gave it a class of A0 IIInn, matching a giant star with "nebulous" lines.

He used to get into the ring with a giant Star of David painted on his shirt, and many young Jews identify with his character. When the rest of the wrestlers returned to the United States, Kozalchik stayed in Poland to start a family. In 1941, the Germans entered the town of Krynica, where he was born and lived. When a 100 kg unexploded bomb was found in a house, Kozalchik picked it up and carried it out of the city.

The brightest component of the system, Sigma Scorpii Aa, is a double-lined spectroscopic binary, which means that the pair has not been resolved using a telescope. Instead, their orbit is determined by changes in their combined spectrum caused by the Doppler shift. This indicates that the pair complete an orbit every 33.01 days and have an orbital eccentricity of 0.32. The primary component of the spectroscopic binary, Sigma Scorpii Aa1, is an evolved giant star with a stellar classification of B1 III.

This is an aging red giant star with a stellar classification of , a star that has used up its core hydrogen and is expanding. The suffix notation indicates there are unusually strong lines of cyanogen in the spectrum. 20 Cyg is listed as one of the least variable stars in the Hipparcos catalogue, changing its brightness by no more than 0.01 magnitude. It has 1.28 times the mass of the Sun and has expanded to 13 times the Sun's radius.

This is an aging giant star with a stellar classification of K0+III, having exhausted the supply of hydrogen at its core and expanded to 11 times the Sun's radius. It is a red clump giant, which means it is on the horizontal branch and is generating energy through helium fusion at its core. The star has 1.8 times the mass of the Sun and is radiating 59 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,750 K.

Xi Orionis (ξ Orionis) is a binary star system in the northeastern part of the constellation of Orion, well above the red giant star, Betelgeuse in the sky. It lies next to another blue main-sequence star, Nu Orionis which is somewhat closer at 520 light years. The apparent visual magnitude of Xi Orionis is 4.47, which is bright enough to be seen with the naked eye. The distance to this star, as determined using the parallax method, is roughly 610 light years.

This is an evolved K-type giant star with a stellar classification of K5 III. It is a suspected variable with an amplitude of 0.03 magnitude. The measured angular diameter of the star after correcting for limb darkening is , which, at the estimated distance of this star, yields a physical size of about 46 times the radius of the Sun. The star is radiating around 560 times the solar luminosity from its outer atmosphere at an effective temperature of 3,940 K.

Judging from changes to its proper motion, there is a chance that this is an astrometric binary. This is an evolved K-type giant star with a stellar classification of K0 III. It is a red clump giant on the horizontal branch of the Hertzsprung–Russell diagram, indicating that is it now generating energy through the thermonuclear fusion of helium at its core. The star has more than twice the mass of the Sun and has expanded to 10 times the Sun's radius.

Its traditional name means "breast" and refers to its position in the constellation. Delta Cygni (the proper name is Fawaris) is another bright binary star in Cygnus, 171 light-years with a period of 800 years. The primary is a blue-white hued giant star of magnitude 2.9, and the secondary is a star of magnitude 6.6. The two components are visible in a medium-sized amateur telescope. The fifth star in Cygnus above magnitude 3 is Aljanah, designated Epsilon Cygni.

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With a stellar classification of G9 II-III, this is an evolved giant star that is radiating 132 times the luminosity of the Sun from its outer envelope at an effective temperature of 4,925 K. At this heat, the star glows with the yellow hue of a G-type star. The radius of this star, as measured using interferometry, is about 18 times the Sun's radius. It has an estimated 4.2 times the mass of the Sun and is around old.

It is most likely (98% chance) a member of the thin disk population. This is an evolved G-type giant star with a stellar classification of G9 III:, where the ':' indicates some uncertainty about the classification. (Bartkevicius and Lazauskaite (1997) classify it as K0 III.) The star has 1.61 times the mass of the Sun and has expanded to about 10 times the Sun's radius. The abundance of iron is lower than in the Sun: the star is considered metal deficient.

Epsilon Piscium (Epsilon Psc, ε Piscium, ε Psc) is the Bayer designation for a star approximately away from the Earth, in the constellation Pisces. It is a yellow-orange star of the G9 III or K0 III spectral type, meaning it has a surface temperature around 5,000 kelvins. This is a normal giant star, slightly cooler in surface temperature, yet brighter and larger than the Sun. It is a suspected occultation double, with both stars having the same magnitude, separated by 0.25 arcsecond.

17 Persei is a single star in the northern constellation of Perseus, located about 390 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.53. This object is moving further from the Earth at a heliocentric radial velocity of +13 km/s. Based upon a stellar classification of K5+III, this is an evolved giant star that has exhausted the hydrogen at its core.

It is moving away from the Sun with a radial velocity of +12.3 km/s. A stellar classification of B8 III/IV suggests it is an evolving B-type star showing mixed traits of a subgiant or giant star. It is a PGa star – a higher temperature variety of the class of chemically peculiar stars known as mercury-manganese stars (HgMn stars). That is, it displays a rich spectra of singly-ionized phosphorus and gallium, in addition to ionized mercury and manganese.

BC Canis Minoris is a variable star in the equatorial constellation of Canis Minor. It has a reddish hue and is just barely visible to the naked eye with an apparent visual magnitude that fluctuates around 6.30. The distance to this object is approximately 520 light years based on parallax, but it is drifting closer with a radial velocity of −67 km/s. This is an aging red giant star currently on the asymptotic giant branch with a stellar classification of M4/5III.

89 Virginis is a single star in the zodiac constellation of Virgo, located 234 light years from the Sun. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 4.959. The star is moving closer to the Earth with a heliocentric radial velocity of −39 km/s. This is an evolved giant star with a stellar classification of K0 III, having exhausted the hydrogen at its core and expanded away from the main sequence.

The visible component is an evolved G-type giant star with a stellar classification of and a spectrum that displays an underabundance of iron with weak cyanogen lines. It is a red clump star that is generating energy through the fusion of helium at its core. Lambda Pyxidis has double the mass of the Sun and is an estimated 1.3 billion years old. It is radiating 49 times the Sun's luminosity from its photosphere at an effective temperature of 5,126 K.

30 Cygni at top left, with 31 Cygni A and B at lower right 30 Cygni is a class A5III (white giant) star in the constellation Cygnus. Its apparent magnitude is 4.83 and it is approximately 610 light years away based on parallax. The Bayer letter ο (omicron) has been variously applied to two or three of the stars 30, 31, and 32 Cygni. 30 Cygni has sometimes been designated as ο1 Cygni with the other two stars being ο2 and ο3 respectively.

This is a bright giant star with a stellar classification of K2.5 II. It is a slow irregular variable of type LC with a frequency of 0.16585 cycles per day. In the R (red) band, the magnitude of the star ranges from 3.43 down to 3.81. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of GZ Vel, this yields a physical size of about 140 times the radius of the Sun.

Nu Cygni, Latinized from ν Cygni, is a binary star system in the constellation Cygnus. Its apparent magnitude is 3.94 and it is approximately 374 light years away based on parallax. The brighter component is a magnitude 4.07 A-type giant star with a stellar classification of A0III n, where the 'n' indicates broad "nebulous" absorption lines due to rapid rotation. This white-hued star has an estimated 3.6 times the mass of the Sun and about 1.9 times the Sun's radius.

Zeta Piscis Austrini (ζ Piscis Austrini) is an orange-hued star in the southern constellation of Piscis Austrinus. It has an apparent visual magnitude of +6.43, which is near the lower limit of stars that can be seen with the naked eye. Based upon an annual parallax shift of 7.55 mas as seen from the Gaia telescope, the star is located 413 ± 2 light years from the Sun. This is an evolved K-type giant star with a stellar classification of K1 III.

54 Aurigae is a binary star system located around 800 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a dim, blue-white hued star with a combined apparent visual magnitude of 6.02. The system is moving further from the Sun with a heliocentric radial velocity of around +19 km/s. The primary component is a B-type giant star of visual magnitude 6.22 with a stellar classification of B7 III.

It is positioned near the ecliptic and thus is subject to lunar occultations. This is an aging giant star with a stellar classification of K5 III, indicating it has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. The stellar spectrum displays strong lines of cyanogen. It presently has 18 times the radius of the Sun and is radiating 102 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,324 K.

This is a spectroscopic binary system with a close circular orbit taking just 0.945 days to complete. Despite their proximity, this does not appear to be a contact binary system. The orbital plane of the two stars lies near the line of sight, so they form an Algol-type eclipsing binary. The first component of the system is an A-type main sequence star with a stellar classification of A2 V. Its companion is giant star with a classification of K0 III.

It is moving closer to the Earth with a heliocentric radial velocity of −8 km/s. This is an evolved K-type giant star with a stellar classification of K4 III, which indicates it has consumed the hydrogen at its core and expanded. It has an estimated 0.57 times the mass of the Sun but with over 11 times the Sun's radius. The star is radiating 127 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,430 K.

It is moving closer to the Earth with a heliocentric radial velocity of −34 km/s, and is a member of the Wolf 630 moving group of stars that share a common motion through space. This object is an evolved giant star with a stellar classification of K2 III. It is around two million years old with a similar mass as the Sun. With the hydrogen at its core exhausted, the star has expanded to ten times the girth of the Sun.

The inner pair of stars in this system form a spectroscopic binary with a combined magnitude of 5.44 and an orbital period of 1.302 days. The primary component is a giant star with a stellar classification of B8 III. Because the orbital plane is inclined near the line of sight, two form an eclipsing binary system. The eclipse of the primary component causes a 0.04 drop in magnitude, while the eclipse of the secondary results in a decrease of 0.03.

43 Aurigae is a star located 382 light years away from the Sun in the northern constellation of Auriga. It is just bright enough to be barely visible to the naked eye with an apparent visual magnitude of 6.33. The star is moving closer to the Earth with a heliocentric radial velocity of −3.4 km/s. This is an aging giant star with a stellar classification of K2 III, having exhausted the hydrogen at its core and expanded off the main sequence.

65 Aurigae is a binary star system located 252 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a faint, orange hued star with an apparent visual magnitude of 5.12. The primary, designated component A, is an aging giant star with a stellar classification of K0 III. It is 3.31 billion years old and has expanded to 13 times the Sun's radius after exhausting the hydrogen at its core.

It is receding from the Earth with a heliocentric radial velocity of +8.5 km/s. The visible component is an aging giant star with a stellar classification of K4 III, currently on the red giant branch. It is around 5.2 billion years old with 1.27 times the mass of the Sun. With the supply of hydrogen at its core exhausted, the star has expanded to 11 times the radius of the Sun and it shines with 42 times the Sun's luminosity.

The stellar classification of 45 And is B7 III-IV, matching an evolving subgiant/giant star. It has about 5.2 times the Sun's radius and is radiating 414 times the Sun's luminosity from its photosphere at an effective temperature of 12,874 K. This star is most likely single. A companion star was discovered by American astronomer George W. Hough in 1890. As of 2006, the companion was at an angular separation of along a position angle of 225° from the primary.

The system is moving toward the Earth with a heliocentric radial velocity of −1.1 km/s. The visible component is an aging red giant star with a stellar classification of M0 III, which indicates it has consumed the hydrogen at its core and evolved off the main sequence. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of 10 And, this yields a physical size of about 33 times the radius of the Sun.

This is an Am star with a stellar classification of kA7 hA8 mF2 (III) ((Sr II)), showing the calcium K line of an A7 star, the hydrogen lines of an A8 star, and the metal lines of an F2 star. It has the luminosity class of a giant star and does not appear to be variable. The star has twice the mass of the Sun and four times the Sun's radius. It is spinning with a projected rotational velocity of 38 km/s.

The star is drifting closer with a radial velocity of −48 km/s. This is an aging giant star with a stellar classification of , where the suffix notation indicates a mild underabundance of iron in the spectrum. With the supply of core hydrogen exhausted, this star has cooled and expanded off the main sequence – at present it has 10 times the girth of the Sun. It is a red clump giant, which means it is on the horizontal branch undergoing core helium fusion.

With a stellar classification of G9 IIIb, it has the spectrum of an evolved, G-type giant star. It has an estimated age of a billion years and is a red clump star that it is generating energy through helium fusion at its core. The star has about double the mass of the Sun and has expanded to 11 times the Sun's radius. It is radiating 67.6 times the Sun's luminosity from its photosphere at an effective temperature of 4,746 K.

It is moving closer to the Earth with a heliocentric radial velocity of -18 km/s. This is an aging giant star with a stellar classification of G8IIIFe-0.5, having exhausted the supply of hydrogen at its core and evolved away from the main sequence. The suffix notation indicates a mild underabundance of iron in the spectrum. It is a red clump giant, which means it is on the horizontal branch and is generating energy through helium fusion at its core.

This is an evolved K-type giant star with a stellar classification of K3 III. It is a red clump star on the horizontal branch, indicating that it is generating energy through helium fusion at its core. The composition of the stellar atmosphere is similar to the Sun, having roughly the same abundance of iron in its spectrum. The star has an estimated 1.64 times the mass of the Sun and has expanded to nearly 22 times the Sun's radius.

The brighter member, designated component A, is an aging giant star with a stellar classification of K5III. It is reported as a semi-regular variable with magnitude ranging from 4.68 to 4.72 over 141 days, although the General Catalogue of Variable Stars describes this as unconfirmed by subsequent observations. It has the variable star designation CI Orionis, while 31 Orionis is the Flamsteed designation. The magnitude 10.2 companion star, component B, is an F-type main-sequence star with a class of F7V.

The brightest member of NGC 6910 is a blue supergiant with spectral type B2 and apparent magnitude 7.0. It is located at the southeast edge of the cluster. It is also known as HD 194279 or V2118 Cygni and it is a variable star with P Cygni profile. A mag 8.1 star lies at the northwest edge of the cluster and a mag 8.5 O6 giant star (HD 229196 = V2245 Cygni) lies a bit southwest from the line connecting the two brightest stars.

The brighter component is an evolved K-type giant star with a stellar classification of K3 III. The measured angular diameter, after correction for limb darkening, is . At the estimated distance of the star, this yields a physical size of about 31.5 times the radius of the Sun. It has 1.67 times the mass of the Sun and radiates 309 times the solar luminosity from its outer atmosphere at an effective temperature of 4,135 K. The star is about three billion years old.

Beta Scuti is the second brightest at magnitude 4.22, followed by Delta Scuti at magnitude 4.72. Beta Scuti is a binary system, with the primary with a spectral type similar to the Sun, although it is 1,270 times brighter. Delta Scuti is a bluish white giant star, which is now coming at the direction of the Solar System. Within 1.3 million years it will come as close to 10 light years from Earth, and will be much brighter than Sirius by that time.

The primary component is a K-type giant star with a stellar classification of K2 III. This is a candidate mild Barium star with the slight overabundance most likely acquired through accretion from what is now a white dwarf companion. The primary has an estimated 1.83 times the mass of the Sun and has expanded to 14 times the Sun's radius. The effective temperature of the outer atmosphere is 4,560 K, from whence it radiates 79 times the solar luminosity.

HD 17156 c is a plausible extrasolar planet approximately 255 light-years away in the constellation of Cassiopeia. The planet is thought to be orbiting the yellow giant star HD 17156. This planet has a mass of 0.063 Jupiter mass (or 20 Earth masses) and takes about 111.314 days or 0.305 year to orbit the star, classifying the planet as a cool Neptunian planet. This put it in the distance of 0.481 astronomical units or 72.0 gigameters with a moderate eccentricity.

This is an evolved K-type giant star with a stellar classification of K0.5 IIIb. It is about 2.27 billion years and is a red clump star on the horizontal branch, which indicates it is generating energy through helium fusion at its core. The star has 1.7 times the mass of the Sun and has expanded to about 10 times the Sun's radius. It is radiating 45 times the Sun's luminosity from its photosphere at an effective temperature of 4,624 K.

Based upon an annual parallax shift of , it is located at a distance of around from Earth. At that distance, the visual magnitude of the star is diminished by 0.15 from extinction caused by intervening gas and dust. Although Iota Aquilae is listed in star catalogues as a giant star, calculations of its dimension show that in reality it is a main-sequence star. It has nearly five times the mass of the Sun and five to six times the Sun's radius.

27 Monocerotis is a single star located about 318 light years away from the Sun star in the equatorial constellation of Monoceros. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.93. The star is advancing toward the Earth with a heliocentric radial velocity of −28 km/s. This object is an aging giant star, most likely (94% chance) on the red giant branch, with a stellar classification of K2III.

This is a long-period spectroscopic binary with an orbital period of approximately 15,000 days (41 years) and an overall apparent visual magnitude of approximately 3.28. The primary of the spectroscopic binary has a stellar classification of K3 III, indicating that it is a giant star. It most likely evolved from a F-type main sequence star after consuming the hydrogen at its core. The secondary is a relatively faint K-type dwarf, which has been imaged using a stellar coronagraph.

This is an evolved G-type giant star with a stellar classification of G7IIIb Fe–1, where the suffix notation indicates an underabundance of iron found in the spectrum. At the age of 2.4 billion years it has become a red clump giant, meaning it is generating energy through helium fusion at its core. It has an estimated 1.94 times the mass of the Sun and is radiating 44.7 times the Sun's luminosity from its photosphere at an effective temperature of 5,017 K.

Kappa Arae (κ Ara, κ Arae) is the Bayer designation for a single star in the southern constellation of Ara. Based upon parallax measurements, it is approximately distant from Earth, give or take a 30 light-year margin of error. With an apparent visual magnitude of 5.21, this star is faintly visible to the naked eye. This is a giant star with a stellar classification of G8 III; its outer envelope has expanded to about 14 times the radius of the Sun.

HD 173780 is a single star in the northern constellation Lyra, near the southern constellation border with Hercules. It is an orange-hued star that is faintly visible to the naked eye with an apparent visual magnitude of +4.84. This object is located at a distance of approximately 237 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −17 km/s. This is an aging giant star with a stellar classification of K3III.

It has an absolute magnitude of −0.81. This is an aging G-type giant star with a stellar classification of G7.5III, which indicates it has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. It has an estimated 3.6 times the mass of the Sun and has grown to 20 times the Sun's radius. The metallicity, or abundance of elements other than hydrogen and helium, is about the same as in the Sun.

It is a candidate member of the IC 2391 moving group of co-moving stars. This is an aging giant star with a stellar classification of K4III, although Humphreys (1970) found a supergiant class of K3Ib. It is a suspected slow irregular variable of type Lc and its brightness varies from magnitude +4.50 to +4.59 with no periodicity. The star now has 131 times the girth of the Sun, having exhausted the supply of hydrogen at its core then cooled and expanded.

Upsilon2 Hydrae, Latinized from υ2 Hydrae, is a solitary star in the equatorial constellation of Hydra. Visible to the naked eye, it is photometrically stable with an apparent visual magnitude of 4.59. Based upon an annual parallax shift of 10.40 mas as seen from Earth, it is located about 314 light years from the Sun. This is a B-type star with a stellar classification of B9 III-IV, showing partial traits of a subgiant and giant star in its spectrum.

9 Hydrae is a single star in the equatorial constellation of Hydra, located 205 light years away from the Sun. It is visible to the naked eye as a faint, yellow-orange hued star with an apparent visual magnitude of 4.87. This body is moving closer to the Sun with a heliocentric radial velocity of −2 km/s. This is an aging giant star with a stellar classification of , where the suffix notation indicates an overabundance of cyanogen in the spectrum.

Eggen (1995) listed it as a proper motion candidate for membership in the IC 2391 supercluster. This is an aging giant star with a stellar classification of K3 III, which indicates it has exhausted the hydrogen at its core and evolved away from the main sequence. As a consequence, it has expanded to 33 times the radius of the Sun. The star is radiating 267 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,080 K.

HD 240237 b is a super-Jupiter exoplanet orbiting the K-type giant star HD 240237 about 4,900 light-years (1,500 parsecs, or nearly km) away from Earth in the constellation Cassiopeia. It orbits outside of the habitable zone of its star at a distance of 1.9 AU. The exoplanet was found by using the radial velocity method, from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent star. The planet has a mildly eccentric orbit.

Mira (), designation Omicron Ceti (ο Ceti, abbreviated Omicron Cet, ο Cet), is a red giant star estimated to be 200–400 light-years from the Sun in the constellation Cetus. ο Ceti is a binary stellar system, consisting of a variable red giant (Mira A) along with a white dwarf companion (Mira B). Mira A is a pulsating variable star and was the first non-supernova variable star discovered, with the possible exception of Algol. It is the prototype of the Mira variables.

Although HD 93250 is known to be a binary star, individual spectra of the two components have never been observed, although they are thought to be very similar. The spectral type of HD 93250 has variously been given as O5, O6/7, O4, and O3. It has sometimes been classified as a main sequence star and sometimes as a giant star. The Galactic O-Star Spectroscopic Survey has used it as the standard star for the newly created O4 subgiant spectral type.

This is an evolved red giant star with a stellar classification of M2.5 IIIb. It is a semiregular variable that ranges between magnitudes 5.11 and 5.17. Hipparcos mission photometry gives an amplitude variation of 0.0148 in magnitude with a frequency of 11.4 cycles per day. In terms of its right ascension coordinates, φ Pegasi is located very near the line of the vernal equinox and will cross over around the year 3030, due to the precession of the Earth's axis.

HD 15920 is a single star in the northern constellation of Cassiopeia. It has a yellow hue and is visible to the naked eye as a dim point of light with an apparent visual magnitude of 5.17. This object is located at a distance of approximately 268 light years from the Sun based on parallax, but it is drifting closer with a radial velocity of −4 km/s. This object is an aging giant star with a stellar classification of G8III.

This star has a stellar classification of B7 III, matching an aging giant star that has exhausted the supply of hydrogen at its core. It is around 201 million years old and is spinning with a projected rotational velocity of 59 km/s, well below its critical velocity of 335 km/s. The star has 3.9 times the mass of the Sun and is radiating 405 times the Sun's luminosity from its photosphere at an effective temperature of 11,885 K.

It is drifting further away with a heliocentric radial velocity of +12.5 km/s. The primary component is an evolved giant star with a stellar classification of G8 III. It is a periodic variable star, showing a change in brightness with an amplitude of 0.004 magnitude at the rate of 7.50983 times per day. With the supply of hydrogen at its core exhausted, the star has cooled and expanded until now it has 10 times the radius of the Sun.

This is a metal-deficient giant star with a stellar classification of K1 IV. It is a red clump giant, which indicates it is on the horizontal branch and is generating energy through the fusion of helium at its core. The star is 4.58 billion years old with 1.37 times the mass of the Sun. It has 22 times the Sun's radius and is radiating 163 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,314 K.

Zeta Draconis A is a giant star with a stellar classification of B6 III. Compared to the Sun, this star is about 2.5 times larger, 3.5 times more massive, and is radiating 148 times as much luminosity. This energy is being emitted from the star's outer envelope at an effective temperature of nearly 13,400 K. The azimuthal rotation velocity along the equator is at least 55 km/s. The north ecliptic pole is located at right ascension 18h and declination +66.5°.

At its distance, the visual magnitude of Kappa Perseii is diminished by an extinction factor of 0.06 due to interstellar dust. It has a relatively high proper motion totaling 0.230 arcseconds per year. There is a 76.3% chance that it is a member of the Hyades-Pleiades stream of stars that share a common motion through space. With an estimated age of 4.58 billion years, Kappa Perseii Aa is an evolved G-type giant star with a stellar classification of G9.5 IIIb.

It is a red giant of spectral type K2III that is around 54 times the Sun's radius and 930 times its luminosity. Around 4 times as massive as the Sun, it spent much of its life as a main-sequence star of spectral type B5V. Lying to the south of the quadrilateral between Beta and Epsilon Corvi is the orange-hued 6 Corvi, an ageing giant star of spectral type K1III that is around 70 times as luminous as the Sun.

The Cygnus OB2 #8A system contains two massive luminous O class stars in a 21.9 day orbit. The primary is a supergiant and the secondary is a giant star. The two stars are not thought to be exchanging mass and their luminosity classes match the main sequence turnoff in the Cyg OB2 association at around O6. The nearby stars Cyg OB2 #8B, #8C, and #8D, originally thought to be a single star, are all massive and luminous class O stars.

A 20-foot Michelson interferometer mounted on the frame of the 100-inch Hooker Telescope, 1920. One of the first uses of optical interferometry was applied by the Michelson stellar interferometer on the Mount Wilson Observatory's reflector telescope to measure the diameters of stars. The red giant star Betelgeuse was the first to have its diameter determined in this way on December 13, 1920. In the 1940s radio interferometry was used to perform the first high resolution radio astronomy observations.

It has an annual parallax shift of 16.20 mas as seen from Earth, which provides a distance estimate of about 201 light years. Kappa Leonis is moving away from the Sun with a radial velocity of +28 km/s. The primary component is an evolved K-type giant star with a stellar classification of K2 III. It is about the same age as the Sun with an estimated 144% of the Sun's mass and has expanded to 17 times the Sun's girth.

HD 125442 is a single star in the southern constellation of Lupus. Its apparent visual magnitude is 4.78, which can be seen with the naked eye. The distance to HD 125442, as determined from its annual parallax shift of , is 147 light years. This is a F-type subgiant star with a stellar classification of F0 IV, having, at the age of 614 million years, used up the hydrogen at its core and begun the process of evolving into a giant star.

A telescope reveals it is formed by two yellowish stars of magnitudes 4.7 and 5.8 that are 0.9 arcseconds apart. The two stars orbit each other every 262 years and the orbital eccentricity is 0.74. The components are a magnitude 4.7 evolved giant star of spectral type G8III, and a magnitude 5.8 F-type main-sequence star of spectral type F8V. The former has exhausted the hydrogen at its core, causing it to expand to 8 times the Sun's radius.

From 2009 to 2011 she was a Clay Postdoctoral Fellow at the Harvard-Smithsonian Center for Astrophysics in Cambridge (Massachusetts). Since 2012 she is an assistant professor of physics at the Massachusetts Institute of Technology. In 2005 Frebel discovered the star HE 1327-2326, which is the most iron- deficient star, stemming from a time very shortly after the Big Bang. In 2007 she also discovered the red giant star HE 1523-0901, which is about 13.2 billion years old.

HD 112410 is a star in the southern constellation of Musca. It has a yellow hue and is too dim to be readily visible to the average sight, having an apparent visual magnitude of 6.86. The distance to this star is 513 light years based on parallax, and it is drifting further away from the Sun with a radial velocity of 73 km/s. It has an absolute magnitude of 1.22. This is an aging giant star with a stellar classification of G8III.

This is an evolved K-type giant star with a stellar classification of K2 III. The measured angular diameter of this star, after correction for limb darkening, is . At its estimated distance, this yields a physical size of about 27.6 times the radius of the Sun. It has about three times the mass of the Sun and radiates 295 times the solar luminosity from its outer atmosphere at an effective temperature of 4,491 K. Sigma Hydrae is around 430 million years old.

Alpha Lupi is a giant star with a stellar classification of B1.5 III. It has about ten times the mass of the sun (~) yet is radiating 25,000 times the Sun's luminosity. The outer atmosphere has an effective temperature of 21,820 K, which gives it the blue-white glow of a B-type star. In 1956 it was identified as a Beta Cephei variable by Bernard Pagel and colleagues, which means it undergoes periodic changes in luminosity because of pulsations in the atmosphere.

This is a giant star with a stellar classification of K4 III. It is 130 times more luminous than the Sun. Kochab has reached a state in its evolution where the outer envelope has expanded to 42 times the radius of the Sun. This enlarged atmosphere is radiating 390 times as much luminosity as the Sun from its outer atmosphere at an effective temperature of 4,030 K. This heat gives the star the orange-hued glow of a K-type star.

Elnath's absolute magnitude is -1.34, similar to another star in Taurus, Maia in the Pleiades star cluster. Like Maia, β Tauri is a B-class giant with a luminosity 700 times solar. It has evolved away from the main sequence to become a giant star, larger and cooler than when it was on the main sequence. However, being approximately 130 light-years distant compared to Maia's estimated 360 light-years, β Tauri ranks as the second-brightest star in the constellation.

In 2018 the Gaia spacecraft measured a parallax of which is a distance of with an error of only . It has a spectral classification of K1II-III, making it a giant star that has evolved away from the main sequence. The mass is 2–7 times the Sun, while measurements of the star's radius give estimates of 45.5 or 50.4 solar radii. The atmosphere of the star displays short period radial velocity variations with a primary period of 4.89 days.

HD 130144 (or EK Boötis) is a semiregular variable star in the northern constellation of Boötes. The variation in luminosity has an amplitude of 0.38 in magnitude with no apparent periodicity. This is an X-ray source, and was possibly the first M-type giant star to have a magnetic field directly detected. It is considered to be a single star, although there is nearby companion at an angular separation of 0.2023″ along a position angle of 82.2° (as of 2010.4812).

39 Cancri is a star in the constellation Cancer, located about 614 light years from the Sun in the Beehive Cluster (NGC 2632). It is a challenge to see with the naked eye, having an apparent visual magnitude of 6.39. This object is moving further from the Earth with a heliocentric radial velocity of 34 km/s. This is an evolved giant star with a stellar classification of G8+ III-IIIb, indicating it has consumed the hydrogen at its core.

The distance to this star is approximately 258 light years based on stellar parallax, and it is drifting further away with a radial velocity of +6 km/s. This is an aging giant star with a stellar classification of K0III. It is a red clump giant, which indicates it is on the horizontal branch and is generating energy through helium fusion at its core. The star has 2.24 times the mass of the Sun and has expanded to 13.4 times the Sun's radius.

It should achieve perihelion in about two million years, approaching as close as . This is an evolved giant star with a stellar classification of K2 III, having exhausted the supply of hydrogen at its core and moved off the main sequence. It is a suspected variable star, possibly of the micro-variable variety, having an amplitude of less than 0.03 in magnitude. 14 Sagittarii is radiating about 317 times the Sun's luminosity from its photosphere at an effective temperature of around 3,940 K.

It is 0.05 degree north of the ecliptic, so can be occulted by the moon and planets. This is a G-type giant star with a stellar classification of G6/8III. With an estimated age of 282 million years, it is an evolved, thin disk star that is currently on the red horizontal branch. The interferometry-measured angular diameter of this star is , which, at its estimated distance, equates to a physical radius of nearly 16 times the radius of the Sun.

Rho Serpentis, Latinized from ρ Serpentis, is a single star in the Caput section of the equatorial Serpens constellation. It has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude of +4.78. The distance to this star is approximately 375 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −62 km/s. This is an aging giant star with a stellar classification of K4.5III.

The primary component is a magnitude 4.89 K-type star with a stellar classification of K1 III-IV, having a spectrum that shows mixed traits of an evolved subgiant and giant star. It is catalogued as a red clump giant, which would indicate it is generating energy through helium fusion at its core. The star has expanded to six times the Sun's radius and is radiating 16 times the solar luminosity from its photosphere at an effective temperature of 4,742 K.

This is an evolved, G-type giant star with a stellar classification of G9 III. At the estimated age of 420 million years it is a red clump star on the horizontal branch, which indicates it is generating energy through helium fusion at its core. Sigma3 Cancri has 2.8 times the mass of the Sun and has expanded to 10.3 times the Sun's radius. It is radiating 72 times the solar luminosity from its photosphere at an effective temperature of 5,170 K.

At the age of about four billion years, this is an evolved K-type giant star with a stellar classification of . The suffix notation CN0.5 indicates a mild overabundance of cyanogen in the stellar atmosphere. It has 1.38 times the mass of the Sun and has expanded to 19 times the Sun's radius. The star is radiating 132 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,316 K. The projected rotational velocity is too small to be measured.

This is an evolved red giant star with a stellar classification of M0.5 III, currently on the asymptotic giant branch of the Hertzsprung–Russell diagram. This indicates it has consumed the hydrogen at its center and is now generating energy through hydrogen and helium fusion along shells surrounding an inert carbon and oxygen core. It has expanded to 43 times the radius of the Sun and is radiating 372 times the Sun's luminosity from its photosphere at an effective temperature of 3,890 K.

A 1990 study of the star gave it a giant star classification, and modeled it with 1.7 times the mass of the Sun, 2.1 times the Sun's radius, and shining with 9.8 times the Sun's luminosity. Past observations of this star appear to show some indications of short term chromospheric variability as well as radial velocity variations. It has a candidate common proper motion companion at a projected separation of 770 AU. This object has a J band magnitude of 10.72.

Gamma Tauri presents as a spectral class G8 or K0 giant star with an apparent magnitude of +3.65. This star has passed through the main sequence phase is now a red clump giant, meaning it is using nuclear fusion of helium at its core to provide energy. Age estimates for Gamma Tauri range from 430 million to 530 million years. By comparison, the age of the Hyades cluster is about 625 million years with an error margin of 50 million years.

Eta Mensae, Latinized from η Mensae, is the Bayer designation for a solitary, orange-hued star in the southern constellation of Mensa. This object has an apparent visual magnitude of 5.47, which is sufficiently luminous to be faintly visible to the naked eye. Based upon an annual parallax shift of 4.88 mas as seen from Earth, this star is located roughly 670 light years from the Sun. This is an evolved K-type giant star with a stellar classification of K4 III.

Mu Horologii (μ Horologii) is a solitary, yellow-white hued star in the southern constellation of Horologium. It is faintly visible to the naked eye with an apparent visual magnitude of 5.11. Based upon an annual parallax shift of 23.04 mas as seen from Earth, it is located about 141.6 light years from the Sun. This is an evolving F-type star with a stellar classification of F0 III/IV, showing mixed traits of a subgiant and a giant star.

HD 225218 is a quadruple star system in the northern constellation of Andromeda. The primary component, HD 225218 A, is a giant star with a stellar classification of B9III, an apparent magnitude of 6.16, and is a candidate Lambda Boötis star. It has a fainter, magnitude 9.65 companion, HD 225218 B, at an angular separation of 5.2″ along a position angle of 171°. The primary itself has been identified as a binary star system through interferometry, with the two components separated by 0.165″.

27 Hydrae is a member of a triple star system system in the equatorial constellation of Hydra, located 222 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with a combined apparent visual magnitude of 4.82. The system is moving further from the Earth with a heliocentric radial velocity of +25.6 km/s. The magnitude 4.91 primary, component A, is an aging giant star with a stellar classification of K0 III.

Epsilon Boötis, also known as Izar or Pulcherrima, is a close triple star popular with amateur astronomers and the most prominent binary star in Boötes. The primary is a yellow- or orange- hued magnitude 2.5 giant star, the secondary is a magnitude 4.6 blue-hued main-sequence star, and the tertiary is a magnitude 12.0 star. The system is 210 light-years away. The name "Izar" comes from the Arabic word for "girdle" or "loincloth", referring to its location in the constellation.

With an age of about 2.2 billion years, this is an evolved, K-type giant star with a stellar classification of K0 III. It is a red clump star on the horizontal branch, which means it is generating energy through helium fusion at its core. The star has an estimated 1.8 times the mass of the Sun and has expanded to 10 times the Sun's radius. It is radiating 53 times the solar luminosity from its photosphere at an effective temperature of 4,660 K.

Sidus Ludoviciana is an 8th-magnitude giant star in the asterism of the Big Dipper in the constellation Ursa Major, halfway between Mizar and Alcor. It was discovered on 2 December 1722 by Johann Georg Liebknecht, who mistook it for a planet and named it after Louis V, Landgrave of Hesse-Darmstadt. A line- of-sight companion with Mizar and Alcor (with a spectral type similar to the latter), it is roughly four times more distant. It has the spectral type A8/F0 III.

Houk (1978) categorizes the visible component (Beta² Sagittarii A) as an F-type main-sequence star with a stellar classification of F2/3 V. However, Malaroda (1975) lists it as an F-type giant star. It is spinning rapidly with a projected rotational velocity of 155 km/s. This is giving it an oblate shape with an equatorial bulge that is 22% larger than the polar radius. Beta² Sagittarii has an estimated 1.4 times the mass of the Sun and is around 933 million years old.

47 arcseconds, it is located roughly from the Sun. If the star were at a distance of , it would have a magnitude of +0.4 and be the third- brightest star in the night sky. This star has a stellar classification of G9 III, which indicates it is an evolved G-type giant star. It has an estimated 172% of the Sun's mass and has expanded to 12 times the radius of the Sun, from which it is shining with 64.6 times the solar luminosity.

Mu Leonis is an evolved K-type giant star with a stellar classification of . The trailing notation indicates that, for a star of its type, it has stronger than normal absorption lines of cyanogen and calcium in its spectrum. It has around 1.5 times the Sun's mass, but has expanded to around 14 times the Sun's radius. Mu Leonis shines with 63 times the luminosity of the Sun from an outer atmosphere that has an effective temperature of 4,436 K. It is around 3.35 billion years old.

This is a K-type giant star with a stellar classification of K4.5 III. It is a suspected variable star with a reported magnitude range of 4.28−4.34. The interferometry-measured angular diameter of this star, after correcting for limb darkening, is , which, at its estimated distance, equates to a physical radius of nearly 45 times the radius of the Sun. It shines with around 472 times the luminosity of the Sun, from an outer atmosphere that has an effective temperature of 3,900 K.

6 Sagittarii has a peculiar velocity of , which may indicate it is a runaway star. This is an evolved giant star with a stellar classification of K2 III. It is only 25 million years old and has around ten times the mass of the Sun. The star is radiating about 6,817 times the Sun's luminosity from its photosphere at an effective temperature of 3,778 K. It appears to be a source of extended infrared excess, but this emission may be due to intervening cirrus.

The visible component is an aging red giant star on the asymptotic giant branch with a stellar classification of M3III. It is a suspected variable, probably semiregular, with its magnitude varying from 4.63 to 4.69 over periods of 37.4 and 118.9 days. With the supply of hydrogen exhausted at its core, the star has cooled and expanded to around 98 times the Sun's radius. It is radiating 960 times the luminosity of the Sun from its bloated photosphere at an effective temperature of 3,882 K.

HD 12055 is a candidate astrometric binary star system in the southern constellation of Phoenix, near the eastern constellation border with Eridanus. It is yellow in hue and is visible to the naked eye with an apparent visual magnitude of 4.82. The system is located at a distance of approximately 249 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +13 km/s. The visible component is an aging giant star with a stellar classification of G6III-IIIb.

24 Persei is a star in the northern constellation of Perseus, located around 337 light years from the Sun. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.94. The object is moving closer to the Earth with a heliocentric radial velocity of −37 km/s. This is an aging giant star with a stellar classification of K2 III, which indicates it has exhausted the hydrogen at its core and evolved away from the main sequence.

About 4° to the north of Gamma Persei is the radiance point for the annual Perseid meteor shower. This is a wide eclipsing binary system with an orbital period of 5,329.8 days (14.6 years). This eclipse was first observed in 1990 and lasted for two weeks. During an eclipse, the primary passes in front of the secondary, causing the magnitude of the system to decrease by 0.55. The primary component of this system is a giant star with a stellar classification of G9 III.

The cluster is estimated to be 94.2 million years old. Cluster members show a slightly higher abundance of elements heavier than helium compared to the Sun; what astronomers refer to as the metallicity. 120 stars, ranging down to visual magnitude 15.1, have been identified as most likely cluster members. Most of the bright stars in this cluster are hot, blue B-type stars but the brightest member is a K-type orange giant star, BM Scorpii, which contrasts sharply with its blue neighbours in photographs.

SS Aurigae is a very close binary star with a period of 4 hours and 20 minutes. Both components are small subdwarf stars; there has been dispute in the scientific community about which star originates the outbursts. UU Aurigae is a variable red giant star at a distance of 2,000 light-years. It has a period of approximately 234 days and ranges between magnitudes 5.0 and 7.0. The Flaming Star Nebula (IC 405), and its neighbor IC 410, along with AE Aurigae, which illuminates the nebula.

A type Ia supernova (read: "type one-A") is a type of supernova that occurs in binary systems (two stars orbiting one another) in which one of the stars is a white dwarf. The other star can be anything from a giant star to an even smaller white dwarf.HubbleSite - Dark Energy - Type Ia Supernovae Physically, carbon–oxygen white dwarfs with a low rate of rotation are limited to below 1.44 solar masses (). Beyond this "critical mass", they reignite and in some cases trigger a supernova explosion.

This is a single-lined spectroscopic binary system with an orbital period of and an eccentricity of 0.13. The a sin i value is , where a is the semimajor axis and i is the orbital inclination to the line of sight from the Earth. The system is a source for X-ray and far-UV emission, with the latter most likely coming from the companion. The primary component is an aging red giant star on the asymptotic giant branch with a stellar classification of M4.5 III.

This is an evolved red giant star with a stellar classification of M1 IIIa. The measured angular diameter of this star is . At the estimated distance of this star, this yields a physical size of about 56 times the radius of the Sun. It is radiating roughly a thousand times the luminosity of the Sun from its outer atmosphere at an effective temperature of 3,900 K. Unexpectedly for a red giant, Pi Geminorum was found to be an X-ray source during the ROSAT all-sky survey.

Because of this instability and history of outbursts, Eta Carinae is considered a prime supernova candidate for the next several hundred thousand years because it has reached the end of its estimated million-year life span. NGC 2516 is an open cluster that is both quite large (approximately half a degree square) and bright, visible to the unaided eye. It is located 1100 light-years from Earth and has approximately 80 stars, the brightest of which is a red giant star of magnitude 5.2.

There are four bright stars in Chamaeleon that form a compact diamond-shape approximately 10 degrees from the South Celestial Pole and about 15 degrees south of Acrux, along the axis formed by Acrux and Gamma Crucis. Alpha Chamaeleontis is a white-hued star of magnitude 4.1, 63 light- years from Earth. Beta Chamaeleontis is a blue-white hued star of magnitude 4.2, 271 light-years from Earth. Gamma Chamaeleontis is a red-hued giant star of magnitude 4.1, 413 light-years from Earth.

This is an aging K-type giant star with a stellar classification of K4III, having exhausted the supply of hydrogen at its core then cooled and expanded to its current size of 46 times the Sun's radius. It is a candidate periodic microvariable, with its brightness fluctuating by 0.005 magnitude at the rate of 0.25664 cycles per day. The star is 1.4 times as massive as the Sun and is radiating 486 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,990 K.

This is an evolved K-type giant star with a stellar classification of K4 III. It has an estimated 1.25 times the mass of the Sun and, at the age of 5.6 billion years, has expanded to about 37 times the Sun's radius. From this enlarged photosphere, it is radiating 186 times the Sun's luminosity at an effective temperature of 4,126 K. It has a magnitude 12.02 visual companion at an angular separation of 209.30 arc seconds along a position angle of 298°, as of 2012.

At that range, the visual magnitude of the star is diminished by an extinction of due to interstellar dust. It is moving further from the Earth with a heliocentric radial velocity of +19 km/s. This is an aging red giant star with a stellar classification of M2.5 III, which indicates it has exhausted the hydrogen at its core and evolved away from the main sequence. It is a suspected variable star that may vary in brightness with an amplitude of 0.07 in magnitude.

This is an evolved K-type giant star with a stellar classification of , showing overabundances of CN and CH molecules in the spectrum. It is a red clump giant, which indicates is on the horizontal branch generating energy via helium fusion at its core. The star is about 288 million years old with 3.5 times the mass of the Sun and 15 times the Sun's radius. It is radiating 87 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,909 K.

3 Equulei is an evolved giant star with a stellar classification of K5 III. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of Delta Ophiuchi, this yields a physical size of about 63 times the radius of the Sun. It is radiating an estimated 949 times the luminosity of the Sun from this expanded outer envelope at an effective temperature of 3,893 K. At this heat, it shines with the orange-hued glow of a K-type star.

This is an aging giant star with a stellar classification of G8 III, having consumed the hydrogen at its core and evolved off the main sequence. It is a red clump giant, which means it is generating energy via helium fusion at its core. The star is 1.50 billion years old with 2.3 times the mass of the Sun, and has expanded to 12 times the Sun's radius. It is radiating 93 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,920 K.

It is moving closer to the Earth with a heliocentric radial velocity of −2 km/s. This is an evolved G-type giant star with a stellar classification of G6 III. The interferometry-measured angular diameter of this star is , which, at its estimated distance, equates to a physical radius of about 12 times the radius of the Sun. It has 3.2 times the mass of the Sun and is radiating 128 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,210 K.

It is drifting further away with a radial velocity of +19 km/s. This evolved object has received stellar classifications of A7Ia and A6II, indicating that it is a massive supergiant or bright giant star. It has 7.8 times the mass of the Sun and is around 40 million years old. The star has expanded to nearly 34 times the girth of the Sun and is radiating around 4,140 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 7,977 K.

BD+48 740 is a giant star suspected of having recently engulfed one of its planets. The star has an overabundance of lithium in its atmosphere, a metal that is destroyed by nuclear reactions in stars. Detection of radial velocity variations indicate a companion planet of 1.6 jupiter masses in a highly eccentric orbit, making orbits of other planets unstable. These indications make the discoverers conclude that another planet has recently plunged into the star, been destroyed, and contributed its lithium content to the star.

Zeta Pyxidis (ζ Pyxidis) is a wide binary star system in the southern constellation of Pyxis. It is visible to the naked eye with a combined apparent visual magnitude of +4.88. Based upon an annual parallax shift of 13.35 mas as seen from Earth, it is located around 244 light years from the Sun. The yellow-hued primary, component A, is an evolved G-type giant star with a stellar classification of , where the suffix notation indicating it has anomalously weak lines of cyanogen.

62 Aurigae is a star located 559 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 6.02. This object is moving further from the Earth with a heliocentric radial velocity of +25 km/s. It is an aging giant star with a stellar classification of K2 III, having exhausted the supply of hydrogen at its core then expanded to 22 times the Sun's radius.

66 Aurigae is a single star located approximately 880 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a faint, orange hued star with an apparent magnitude of 5.23. This object is moving further from the Earth with a heliocentric radial velocity of +22.6 km/s. At the age of 107 million years, 66 Aurigae is an evolved giant star, most likely (98% chance) on the horizontal branch, with a stellar classification of K0.5 IIIa.

It is moving closer with a heliocentric radial velocity of −8 km/s. The primary component is an aging red giant star with a stellar classification of . The suffix notation indicates this is a mild barium star, which means the stellar atmosphere is enriched with s-process elements. It is either a member of a close binary system and has previously acquired these elements from a (now) white dwarf companion or else it is on the asymptotic giant branch and is generating the elements itself.

Based upon an annual parallax shift of as seen from Earth orbit, it is located 266 light years away. It is moving closer to the Earth with a heliocentric radial velocity of −21 km/s. This is an evolved giant star with a stellar classification of G7.5 III that is most likely (87% chance) on the red giant branch. As such, it is estimated to be 620 million years old with 2.5 times the mass of the Sun and has expanded to 14 times the Sun's radius.

Based upon an annual parallax shift of 7.53 milliarcseconds, the distance to this star is about . This is an evolved giant star with a stellar classification of K3 III. It has expanded to 37 times the radius of the Sun and is radiating 434 times the luminosity of the Sun from its outer envelope at an effective temperature of 4,170 K. This gives it the orange-hued glow of a K-type star. It is a suspected variable star that ranges in magnitude between 4.66 and 4.71.

Systematic observation for determining the orbit of this system began in 2002, some eighty years following the first radial velocity measurements. It is a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.368. The visible component is an aging giant star with a stellar classification of K1III. At the age of 1.26 billion years old it is a red clump giant, which indicates it is on the horizontal branch and is generating energy through helium fusion at its core.

The star is moving closer with a heliocentric radial velocity of −11 km/s. It has a magnitude 11.7 visual companion at an angular separation of along a position angle of 348°, as of 2002. At the age of 2.2 billion years, this is an aging giant star with a stellar classification of K5 III, having consumed the hydrogen at its core and evolved away from the main sequence. It has 1.6 times the mass of the Sun and has expanded to 26 times the Sun's radius.

The projected semi- major axis of the primary star's orbit is , providing a lower bound on the separation of the stars. The system is around four billion years old. The visible component is an evolved K-type giant star with a stellar classification of ; the suffix notation indicates a mild underabundance of iron in the spectrum. It is probably on the horizontal branch, fusing helium in its core, but may be on the red giant branch fusing hydrogen in a shell around an insert helium core.

It is traversing the sky with a net proper motion of 0.176 arc seconds per year, and has a radial velocity toward the Sun of −25.72 km/s. This star has a stellar classification of K2 III, matching an evolved K-type giant star. It belongs to the so-called "red clump", indicating that it is generating energy through helium fusion at its core. This star is about four billion years old and is spinning with a projected rotational velocity of 3.5 km/s.

Pi Boötis, Latinized from π Boötis, is a probable triple star system in the northern constellation of Boötes. It is visible to the naked eye with a combined apparent visual magnitude of 4.50. Based upon an annual parallax shift of 10.67 mas as seen from Earth, it is located roughly 310 light years from the Sun. The brighter primary, component π1 Boötis, has a visual magnitude of 4.89 and a stellar classification of , which suggests it is an evolved blue-white hued B-type giant star.

This is an aging K-type giant star with a stellar classification of K3 III. It is a red clump giant, which indicates it is on the horizontal branch and is generating energy through helium fusion at its core. The star is around five billion years old with 1.1 times the mass of the Sun and has expanded to 12 times the Sun's radius. It is radiating 52 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,472 K.

39 Eridani is a wide binary star system in the equatorial constellation of Eridanus. It is visible to the naked eye as a faint, orange-hued star with a combined apparent visual magnitude of 4.87. As of 2015, the components had an angular separation of along a position angle of 143°. The system is moving further from the Sun with a heliocentric radial velocity of +7 km/s. The magnitude 5.07 primary, designated component A, is an aging giant star with a stellar classification of K3 III.

81 Geminorum lies close enough to the ecliptic to undergo lunar occultations. The variable velocity of this system was first suspected at the Dominion Astrophysical Observatory in 1921, then confirmed by the Lick Observatory in 1922. It is a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.325. The visible component is an aging giant star with a stellar classification of K4 III, having exhausted the supply of hydrogen at its core then expanded to 34 times the Sun's radius.

The primary, component A, is a variable star, most likely of the slow irregular type, which ranges in magnitude from 4.91 down to 4.96. It is a giant star with a stellar classification of K3 III, which indicates it has exhausted the hydrogen at its core and evolved away from the main sequence. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of this star, this yields a physical size of about 27 times the Sun's radius.

HD 20644 is a suspected binary star system in the constellation Aries. It has an orange hue and is visible to the naked eye with an apparent visual magnitude of 4.47. The system is located at a distance of approximately 540 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −3 km/s. The visible component is an aging giant star with a stellar classification of K3IIIa Ba0.5, where the suffix notation indicates this is a mild barium star.

3 Monocerotis is a binary star system in the equatorial constellation of Monoceros, located approximately 780 light years away from the Sun based on parallax. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.92. The system is moving further from the Earth with a heliocentric radial velocity of +39 km/s. The magnitude 4.98 primary, designated component A, has a stellar classification of B5 III, matching an evolved blue giant star.

Omicron Andromedae is a Gamma Cassiopeiae type variable star and the system's brightness varies from magnitude +3.58 to +3.78. The variable component is the brightest and most massive star in the system, Aa. The spectrum is predominantly that of a B6 giant star, from the brightest component in the system. It is a shell star and the spectrum contains emission lines with variable profiles. Spectral lines similar to an A2 star are also detectable in the spectrum and these are thought to originate in the B component.

Eta Arae, Latinized from η Arae, is the Bayer designation for a single star in the southern constellation of Ara. It is approximately from Earth and is visible to the naked eye with an apparent visual magnitude of 3.76. The star is moving away from the Sun with a radial velocity of +9 km/s. The spectrum of this star matches a stellar classification of K5 III, indicating that, at an estimated age of five billion years, it has reached the giant star stage of its evolution.

This is a yellow K-type giant star with a stellar classification of K0 III. At the age of around 550 million years it has become a red clump star, which indicates it is generating energy via helium fusion at its core. It has an estimated 2.55 times the mass of the Sun and is radiating 48 times the Sun's luminosity from its photosphere at an effective temperature of 4,910 K. The magnitude 11.5 companion lies at an angular separation of , as of 2008.

Sigma Capricorni, Latinized from σ Capricorni, is a solitary star in the southern constellation of Capricornus, located just to the north of the ecliptic. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of +5.31. The star is located approximately 1,070 light years away from the Sun based on parallax, but is drifting closer with a radial velocity of −9.6 km/s. This object is an evolved, K-type giant star with a stellar classification of K2 III.

Lambda Ceti is a blue giant star with stellar classification B6III. With a mass between and an estimated radius that is , the star radiates a bolometric luminosity of about . In 1997 the Hipparcos satellite estimated its parallax at 7.69 ± 0.76 milliarcseconds yielding a distance from Earth of about 130 ± 10 parsecs or 420 ± 40 light years. However recent astrometric calculations by van Leeuwen have placed the distance much farther at about 177 ± 7 pc or 580 ± 20 ly—a revaluation which significantly altered other stellar parameters.

O. J. Eggen identified it as a member of the Pleiades group of co-moving stars. This object is a massive bright giant star with a stellar classification of B5 II. It is 25 million years old and is spinning with a projected rotational velocity of 19 km/s. The star has 9 times the mass of the Sun and about 18 times the Sun's radius. It is radiating 11,634 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 14,300 K.

Eta Draconis A is a star with 2.55 times the mass of the Sun. The spectrum matches a stellar classification of G8 III, with the luminosity class III indicating this is an evolved giant star that has exhausted the supply of hydrogen at its core. It reached this stage in only 550 million years because higher mass stars such as this consume the supply of hydrogen more rapidly than the Sun. The measured angular diameter of this star, after correction for limb darkening, is .

Zeta Gruis, Latinized from ζ Gruis, is a solitary star in the southern constellation of Grus. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.12. Based upon an annual parallax shift of 24.5 mas as seen from the Earth, the system is located about 133 light years from the Sun. This is an evolved K-type giant star with a stellar classification of , where the suffix notation indicates underabundances of iron and cyanogen in the spectrum.

A star whose initial mass is less than approximately will not become a giant star at all. For most of their lifetimes, such stars have their interior thoroughly mixed by convection and so they can continue fusing hydrogen for a time in excess of 1012 years, much longer than the current age of the Universe. They steadily become hotter and more luminous throughout this time. Eventually they do develop a radiative core, subsequently exhausting hydrogen in the core and burning hydrogen in a shell surrounding the core.

HD 39225, also known as HR 2028, is a variable star in the northern constellation Auriga, located around 620 light years away from the Sun. It is visible to the naked eye as a faint, red-hued star with an apparent visual magnitude of around 6.04. This is a suspected runaway star that is moving away from the Sun with a heliocentric radial velocity of 98 km/s. Currently on the asymptotic giant branch, this is an evolved red giant star with a stellar classification of .

26 Hydrae is a binary star system located 334 light years away from the Sun in the equatorial constellation of Hydra. It is visible to the naked eye as a faint, yellow-hued point of light with a combined apparent visual magnitude of 4.77, just a few degrees away from Alphard. The system is moving closer to the Earth with a leisurely radial velocity of -1 km/s. Keenan and McNeil (1989) gave the brighter component a stellar classification of G7 III, matching an aging giant star.

Eggen (1971) listed it as a member of the η Cephei group of old-disk stars. This is an evolved giant star with a stellar classification of K4 III, which indicates it has exhausted the supply of hydrogen at its core and expanded off the main sequence. It has 1.31 times the mass of the Sun but has swollen to 13.5 times the Sun's radius. The star is radiating 55 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,255 K.

The stellar classification of the visible component is , which matches an evolved K-type giant star with a mild overabundance of CN in the atmosphere. At the age of 4.34 billion years, it is a red clump star, which indicates it is on the horizontal branch and is generating energy through helium fusion at its core. The star has 1.55 times the mass of the Sun and is radiating 178 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,415 K.

The star is positioned near the ecliptic and thus is subject to occultation by the Moon. This is an aging K-type giant star with a stellar classification of , which means it has exhausted the hydrogen at its core and evolved away from the main sequence. The suffix notation indicates a mild underabundance of iron in the atmosphere. It has expanded to 37 times the Sun's radius and is radiating over a thousand times the Sun's luminosity from its photosphere at an effective temperature of 4,001 K.

This object is drifting closer with a radial velocity of −13 km/s. This is an evolved red giant star with a stellar classification of M2 III. It is a variable star of uncertain type, showing a change in brightness with an amplitude of 0.0114 magnitude and a frequency of 0.22675 cycles per day, or 4.41 days/cycle. It has about 67 times the Sun's radius and is radiating 975 times the Sun's luminosity from its photosphere at an effective temperature of 3,936 K.

This is an evolved giant star with a stellar classification of K0 III. The interferometry-measured angular diameter of this star, after correcting for limb darkening, is , which, at its estimated distance, equates to a physical radius of about 10.6 times the radius of the Sun. The outer envelope has an effective temperature of 4,980 K, giving it the orange-hued glow of a cool, K-type star. Soft X-ray emission has been detected from this star, which has an estimated X-ray luminosity of .

Overall, there are 41 stars within the constellation's borders with apparent magnitudes brighter than or equal to 6.5. With an apparent magnitude of 3.68, Alpha Pyxidis is the brightest star in the constellation. Located 880 ± 30 light-years distant from Earth, it is a blue-white giant star of spectral type B1.5III that is around 22,000 times as luminous as the Sun and has 9.4 ± 0.7 times its diameter. It began life with a mass 12.1 ± 0.6 times that of the Sun, almost 15 million years ago.

This is an evolved G-type giant star with a stellar classification of G9 III, a star that has used up its core hydrogen and has expanded. At present it has ten times the radius of the Sun and is radiating 52 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,893 K. It has a visual magnitude 12.50 companion, not visible even through binoculars, located at an angular separation of 21.70 arc seconds along a position angle of 74°, as of 2011.

Size comparison between Aldebaran and the Sun Aldebaran is listed as the spectral standard for type K5+ III stars. Its spectrum shows that it is a giant star that has evolved off the main sequence band of the Hertzsprung–Russell diagram after exhausting the hydrogen at its core. The collapse of the centre of the star into a degenerate helium core has ignited a shell of hydrogen outside the core and Aldebaran is now on the red giant branch (RGB). The effective temperature of Aldebaran's photosphere is .

They are all considered to be cataclysmic variable stars. Classical nova eruptions are the most common type. They are likely created in a close binary star system consisting of a white dwarf and either a main sequence, subgiant, or red giant star. When the orbital period falls in the range of several days to one day, the white dwarf is close enough to its companion star to start drawing accreted matter onto the surface of the white dwarf, which creates a dense but shallow atmosphere.

Because the star lies near the ecliptic it is subject to occultations by the Moon, allowing the angular size to be measured. As of 1940, the pair had an angular separation of 0.10 arc seconds along a position angle of 191°. The yellow-hued primary, component Aa, is an evolved G-type giant star with a stellar classification of G8.5 III and an estimated age of 4.3 billion years. It has 1.15 times the mass of the Sun and has expanded to 11.14 times the Sun's radius.

Zeta Ceti is a single-lined spectroscopic binary system with an orbital period of 4.5 years and an eccentricity of 0.59. The primary, Baten Kaitos, is an evolved K-type giant star with a stellar classification of . The suffix notation indicates this is a weak barium star, showing slightly stronger than normal lines of singly-ionized barium. This star has an estimated 2.34 times the mass of the Sun and, at an estimated age of 1.24 billion years, has expanded to 25 times the Sun's radius.

This is known to be a spectroscopic binary system, although there is no information about the secondary component. Based upon parallax measurements, this system is located at a distance of about from the Earth. The spectrum of the primary star matches a stellar classification of A9III, which indicates this is a giant star that has exhausted the hydrogen at its core and evolved away from the main sequence. The effective temperature is about 7,031 K, giving the star a white hue characteristic of A-type stars.

Delta Arietis is an evolved giant star with a stellar classification of K2 III. It belongs to a population known as red clump giants, which means it is generating energy through the fusion of helium at its core. With close to twice the mass of the Sun, the outer envelope has expanded until it is around ten times the Sun's radius. It shines with 45 times the Sun's luminosity at an effective temperature of 4,810 K, giving it the orange-hued glow of a K-type star.

Lambda Draconis (λ Draconis, abbreviated Lam Dra, λ Dra), also named Giausar , is a solitary, orange-red star in the northern circumpolar constellation of Draco. It is visible to the naked eye with an apparent visual magnitude of +3.85. Based upon an annual parallax shift of 9.79 mas as seen from the Earth, the star is located around 333 light years from the Sun. This is an evolved red giant star on the asymptotic giant branch with a stellar classification of M0III-IIIa Ca1.

The primary, component A, is a magnitude 5.85 B-type star with a stellar classification of B8 III-IVe, suggesting it may be part way along the path of evolving into a giant star from a subgiant. It has about 3.6 times the mass of the Sun and 4.4 times the Sun's radius, although it may be tidally deformed since its radius is 86% of the Roche radius. With an estimated age of 158 million years, it has a projected rotational velocity of 112 km/s.

The visible component is an evolved giant star with a stellar classification of , where the suffix notation indicates an underabundance of iron in the spectrum. It has 1.5 times the mass of the Sun and has expanded to 7 times the Sun's radius. The star is radiating 26 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,920 K. It has a magnitude 10.49 visual companion at an angular separation of along a position angle of 57°, as of 2004.

Artist's impression of R Aquarii, a symbiotic binary, during an active phase A symbiotic binary is a type of binary star system, often simply called a symbiotic star. They usually contain a white dwarf with a companion red giant. The cool giant star loses material via Roche lobe overflow or through its stellar wind, which flows onto the hot compact star, usually via an accretion disk. Symbiotic binaries are of particular interest to astronomers as they can be used to learn about stellar evolution.

G 99-47's mass is 0.71 ± 0.03 Solar masses; its surface gravity is 108.20 ± 0.05 (1.58 · 108) cm·s−2, or approximately 162 000 of Earth's, corresponding to a radius 7711 km, or 121% of Earth's. Its temperature is 5790 ± 110 K, almost like the Sun's; its cooling age, i. e. age as degenerate star (not including lifetime as main sequence star and as giant star) is 3.97 Gyr. Due almost equal to the Sun's temperature, GJ 1087 should appear almost the same color as the Sun.

40 Camelopardalis is a single star in the northern circumpolar constellation of Camelopardalis, located around 600 light years distant from the Sun. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.37. This object is moving further from the Earth with a heliocentric radial velocity of +8.6 km/s. This is an aging giant star with a stellar classification of K3 III, having exhausted the hydrogen at its core and evolved away from the main sequence.

Telescopium is a minor constellation in the southern celestial hemisphere, one of twelve named in the 18th century by French astronomer Nicolas-Louis de Lacaille and one of several depicting scientific instruments. Its name is a Latinized form of the Greek word for telescope. Telescopium was later much reduced in size by Francis Baily and Benjamin Gould. The brightest star in the constellation is Alpha Telescopii, a blue-white subgiant with an apparent magnitude of 3.5, followed by the orange giant star Zeta Telescopii at magnitude 4.1.

With an annual parallax shift of 9.24 mas as viewed from Earth, Zeta Crateris is located roughly 350 light years from the Sun. At that distance, the visual magnitude of the system is diminished by an extinction factor of 0.21 due to interstellar dust. The two components of this system had an angular separation of 0.20 arc seconds along a position angle of 22°, as of 1991. The primary, component A, is a magnitude 4.95 evolved giant star with a stellar classification of G8 III.

They are drifting closer to the Earth with a heliocentric radial velocity of −6 km/s. The primary, designated component A, is an aging giant star with a stellar classification of G8 III, but has most likely not yet made multiple ascents up the red giant branch. It has 3.11 times the mass of the Sun and has expanded to 14 times the Sun's radius. The star is radiating 210 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 5,058.

This is a single, orange-hued star with a stellar classification of K2 III, indicating it is an evolved K-type giant star. It is a red clump star, which means it is on the horizontal branch and is generating energy through helium fusion at its core. The stellar mass has been estimated via astroseismology, giving a value of 1.6 times the mass of the Sun. It is radiating about 41 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,546 K.

The maximum value of the sine function is 1.0; hence, 'a' is no smaller than the value cited. The visible component appears to be an evolved giant star with a stellar classification of , where the suffix notation indicates an underabundance of iron in the atmosphere. It is 320 million years old with 3.27 times the mass of the Sun and about 13 times the Sun's radius. The star is radiating 219 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,024 K.

It is moving further from the Sun with heliocentric radial velocity of +42.6 km/s. This is an evolved G-type giant star with a stellar classification of G8 IIIb. At the age of around 550 million years old, it is a red clump giant, which means it has already undergone helium flash and is generating energy through helium fusion at its core. The star has an estimated 2.5 times the mass of the Sun and has expanded to 8.7 times the Sun's radius.

This is an aging giant star with a stellar classification of K5 III, indicating it has exhausted the hydrogen at its core and evolved off the main sequence. It is a suspected variable star of unknown type. The interferometry-measured angular diameter of the primary component, after correcting for limb darkening, is , which, at its estimated distance, equates to a physical radius of about 54 times the radius of the Sun. It is around 1.15 billion years old with 1.4 times the mass of the Sun.

57 Cancri is a double star in the zodiac constellation of Cancer, located around 460 light years away from the Sun. They are visible to the naked eye as a faint star with a combined apparent visual magnitude of +5.40. The brighter member, designated component A. is a yellow-hued giant star with a stellar classification of G7 III and an apparent magnitude of +6.09. Its companion, component B, is an orange-hued giant with a class of K0 III and an apparent magnitude of +6.37.

13 Cancri (abbreviated to 13 Cnc) is a K-type giant star in the constellation Cancer. It has an apparent magnitude of +6.41 and is approximately 970 light years from Earth. Its designation is unusual as it is one of a very few stars which have a Bayer designation and are not in the Bright Star Catalog, although the designation ψ1 Cancri is rarely used. It is one of the few stars with a Flamsteed designation that are not listed in the Bright Star Catalogue.

At an age of about 3.58 billion years, Lambda2 Sculptoris is an evolved red clump giant star with a stellar classification of K0 III. It is presently on the horizontal branch and is generating energy through the nuclear fusion of helium at its core. The star has an estimated 1.49 times the mass of the Sun and has expanded to about 14 times the Sun's radius. It is radiating 63 times the solar luminosity from its photosphere at an effective temperature of 4,531 K.

54 Eridani is a suspected astrometric binary star system located around 400 light years from the Sun in the equatorial constellation of Eridanus. It is visible to the naked eye as a faint, reddish hued star with a baseline apparent visual magnitude of 4.32. The object is moving closer to the Earth with a heliocentric radial velocity of −33 km/s. The visible component is an aging red giant star, currently on the asymptotic giant branch, with a stellar classification of M3/4 III.

7 Comae Berenices is a single star located 249 light years away in the northern constellation of Coma Berenices. It is a dim star but visible to the naked eye near the Coma Star Cluster with an apparent visual magnitude of 4.93. The star is moving closer to the Earth with a heliocentric radial velocity of −28 km/s, and is predicted to come as close as in 2.4 million years. This is an evolved giant star with a stellar classification of G8 III–IIIb.

The planet orbits a (K-type) giant star named Kepler-432 A. It has exhausted the hydrogen in its core and has begun expanding into a red giant. The star has a mass of 1.32 and a radius of 4.06 . It has a surface temperatures of 4995 K and is 4.2 billion years old. In comparison, the Sun is about 4.6 billion years old and has a surface temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.

Kepler-432b (also known by its Kepler Object of Interest designation KOI-1299.01) is a hot super-Jupiter (or "warm" super-Jupiter) exoplanet orbiting the giant star Kepler-432 A, the innermost of two such planets discovered by NASA's Kepler spacecraft. It is located about 2,830 light-years (870 parsecs, or nearly km) from Earth in the constellation Cygnus. The exoplanet was found by using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured.

This is an F-type subgiant star with a stellar classification of F0 IV. However, Malaroda (1975) gave a classification of F2 III, which would indicate a more evolved giant star. It is estimated to have nearly double the mass of the Sun with 3.1 times the Sun's radius. The star is around 1.1 billion years old and has a projected rotational velocity of 63.5 km/s. It is radiating 23 times the luminosity of the Sun from its photosphere at an effective temperature of 7,166 K.

Epsilon Scorpii (ε Scorpii, abbreviated Eps Sco, ε Sco), formally named Larawag , is a star in the southern zodiac constellation of Scorpius. It has an apparent visual magnitude of +2.3, making it the fifth-brightest member of the constellation. Parallax measurements made during the Hipparcos mission provide an estimated distance to this star of around from the Sun. Epsilon Scorpii has a stellar classification of K1 III, which indicates it has exhausted the supply of hydrogen at its core and evolved into a giant star.

HD 895 is a multiple star system in the constellation Andromeda. Its apparent magnitude is 6.277, so it can be seen by the naked eye under very favourable conditions. Based on parallax measured by Hipparcos, the system is located around away, and it's made of two different spectroscopic binary pairs. The first pair is made of a primary yellow giant star of spectral type G0III, and the secondary subgiant star of spectral type K2IV, so they have both left the main sequence evolutionary phase.

R Microscopii is a star in the constellation Microscopium. It is a red giant star of spectral type M4e that is also a Mira variable, with an apparent magnitude ranging between 8.3 and 13.8 over 138 days. Located around 1000 light-years distant, it shines with a luminosity 444 times that of the Sun and has a surface temperature of 3141 K. The Astronomical Society of Southern Africa in 2003 reported that observations of R Microscopii were urgently needed as data on its light curve was incomplete.

The stellar classification of HD 14622 is F0 III–IV, showing a mixed spectrum of an evolving subgiant and giant star; suggesting this is an intermediate-mass star that has used up its core hydrogen and is expanding. The star is suspected of being slightly variable, but this has not been conclusively proven. It is around 890 million years old with 1.69 times the mass of the Sun. The star is radiating 8 times the Sun's luminosity from its photosphere at an effective temperature of approximately 7,000.

CG Andromedae is also a chemically peculiar star with a strong magnetic field, or Ap star, with a spectral type A0IIspSiSrHg. This means that it's a bright giant star that shows narrow absorption lines and unusual strong lines of silicium, strontium and mercury. Calcium and manganese lines are weaker than expected instead. Other sources report that the stronger lines are of silicium and europium, thus giving a spectral classification B9pSiEu, which has just a slightly different temperature for the blackbody emission in addition to the different lines.

This is an aging red giant star with a stellar classification of M3 III, indicating that it has consumed the hydrogen at its core and evolved away from the main sequence. Eggen lists it as being on the asymptotic giant branch. It has been classified as a semiregular variable of type SRb, ranging from magnitude 5.18 down to 5.31 with periods of 360 and possibly 22 days. It shines with a luminosity approximately 536 times that of the Sun and has an effective temperature of 3,779 K.

Phi Sagittarii (Phi Sgr, φ Sagittarii, φ Sgr) is a star in the southern constellation of Sagittarius. With an apparent visual magnitude of 3.17, it is the ninth-brightest star in the constellation and is readily visible to the naked eye. Parallax measurements place it at a distance of roughly from the Earth. The stellar classification of this star has been rated at B8.5 III and B7 IV, with a luminosity class of III indicating it is a giant star, while a class of IV suggests it is still a subgiant star.

This is an aging giant star with a stellar classification of K0 III, a star that has used up its core hydrogen and has expanded. It is a red clump giant on the horizontal branch, which indicates it is generating energy through the fusion of helium at its core. 11 Serpentis is 2.75 billion years old with 1.3 times the mass of the Sun and has 11 times the Sun's radius. It is radiating 50 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,767 K.

The primary and secondary are close together but the primary and tertiary are widely separated. Omicron Cassiopeiae is a triple star and the primary is another γ Cassiopeiae variable. Sigma Cassiopeiae is a binary star 1500 light-years from Earth. It has a green-hued primary of magnitude 5.0 and a blue-hued secondary of magnitude 7.3. Psi Cassiopeiae is a triple star 193 light-years from Earth. The primary is an orange-hued giant star of magnitude 4.7 and the secondary is a close pair of stars that appears to be of magnitude 9.0.

10 Serpentis is a single, white-hued star in Serpens Caput, the western section of the equatorial constellation of Serpens. It is faintly visible to the naked eye with an apparent visual magnitude of 5.15. Located around distant, it is moving closer to the Sun with a heliocentric radial velocity of −10 km/s and will make its closest approach in around 983,000 years at a separation of about . Abt and Morrell (1995) gave this star a stellar classification of A6 III, matching an evolved red giant star that has used up its core hydrogen.

This is an aging red giant star with a stellar classification of K1III, a star that has used up its core hydrogen and has expanding. It is a candidate horizontal branch star, which would indicate it is past the red giant branch stage and is fusing helium at its core. The star is nearly four billion years old with 1.4 times the mass of the Sun and 3.7 times the Sun's radius. It is radiating eight times the luminosity of the Sun from its photosphere at an effective temperature of 5,028 K.

This is an aging K-type giant star with a stellar classification of K3 III, which means it has exhausted the supply of hydrogen at its core. There is a 57% chance that this evolved star is on the horizontal branch and a 43% chance it is still on the red-giant branch. If it is on the former, the star is estimated to have 1.09 times the mass of the Sun, nearly 27 times the solar radius and shines with 191 times the Sun's luminosity. It is around 8 billion years old.

S Canis Minoris is a variable star in the equatorial constellation Canis Minor. It has a peak apparent visual magnitude of , which lies below the minimum brightness that is normally visible to the naked eye. The star is located at a distance of approximately 1,600 light-years from the Sun based on stellar parallax, and is drifting further away with a radial velocity of about +68 km/s. This is an aging red giant star with a stellar classification of M7-8e, where the 'e' suffix indicates emission lines in the spectrum.

Chi Pegasi, Latinized from χ Pegasi, is a single star in the northern constellation of Pegasus, along the eastern constellation border with Pisces. It has a reddish hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.80. The distance to this star is approximately 368 light years based on parallax, but it is drifting closer with a radial velocity of -46 km/s. This is an aging red giant star on the asymptotic giant branch with a stellar classification of M2+III.

Gamma Piscium (Gamma Psc, γ Piscium, γ Psc) is a star approximately 138 light years away from Earth, in the zodiac constellation of Pisces. It is a yellow star with a spectral type of G8 III, meaning it has a surface temperature of 4,833 K and is a giant star. It is slightly cooler than the Sun, yet it is 11 solar radii in size and shines with the light of 63 Suns. At an apparent magnitude of 3.7, it is the second brightest star in the constellation Pisces, between Eta and Alpha.

54 Persei is a single star in the northern constellation of Perseus. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 4.93. The star is located approximately 220 light years away based on parallax, but is drifting closer with a radial velocity of −27 km/s. This is an aging giant star with a stellar classification of G8+ IIIb, a star that has exhausted the supply of hydrogen at its core and expanded to more than nine times the girth of the Sun.

Grotius assigned the name Isis to this star, but the name, now obsolete, belonged rather to Gamma Canis Majoris. As of 2011, the pair had an angular separation of 2.77 arc seconds along a position angle of 343.9°. The orange-hued primary member, component A, is an evolved K-type giant star with a stellar classification of K2/3 III and a visual magnitude of 5.27. The base magnitude 7.32 companion, component B, is a hybrid B/A-type main-sequence star with a class of B9/A0 V. The system has two visual companions.

Information about the previous use of the land or the different construction projects on the land is scarce; however, some important details can be seen in an aerial shot. For example, the design shown in the undated picture shows a giant star made into the ground, with the plaza's stage at the center. The red point of the star that points straight to the U.S. Embassy a few hundred feet away is most clear. As of May 2006, the plaza includes a stage, metal arches over the crowd area, and a monument of 138 flags.

At the age of one billion years, this is an evolved giant star with a stellar classification of K0− III, which means it has used up its core hydrogen and expanded. It is a red clump giant, indicating that it is on the horizontal branch of the Hertzsprung–Russell diagram and is generating energy by helium fusion at its center. The star has double the mass of the Sun and eight times the Sun's radius. It is radiating 45 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,983 K.

The brighter magnitude 5.18 primary is an aging red giant star with a stellar classification of M1IIIab. Having exhausted the supply of hydrogen at its core, it has expanded to around 45 times the radius of the Sun. It is a suspected variable star of unknown type and amplitude. The star is radiating 439 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,954 K. An optical companion, with a spectral type of K, is a few arcseconds away and has an apparent magnitude of 10.14.

The constellation's brightest star—and the only one brighter than an apparent magnitude of 4—is Alpha Horologii (at 3.85), an ageing orange giant star that has swollen to around 11 times the diameter of the Sun. The long-period variable-brightness star, R Horologii (4.7 to 14.3), has one of the largest variations in brightness among all stars in the night sky visible to the unaided eye. Four star systems in the constellation are known to have exoplanets; at least one—Gliese 1061—contains an exoplanet in its habitable zone.

Eta Columbae is a solitary star near the southern boundary of the constellation Columba. It is visible to the naked eye, having an apparent visual magnitude of 3.96. Based upon an annual parallax shift of 6.91 mas, it lies at a distance of roughly 472 light years from the Sun. This is an orange- hued K-type giant star with a stellar classification of K0 III, or possibly a bright giant with a crossover class of G8/K1 II. The measured angular diameter of this star, after correction for limb darkening, is .

Thus the age of a single population cluster can be measured by looking for the stars that are just beginning to enter the giant star stage. This forms a "knee" in the HR diagram, bending to the upper right from the main-sequence line. The absolute magnitude at this bend is directly a function of the age of globular cluster, so an age scale can be plotted on an axis parallel to the magnitude. In addition, globular clusters can be dated by looking at the temperatures of the coolest white dwarfs.

Flanking Alpha to the east is Gamma Coronae Borealis, yet another binary star system, whose components orbit each other every 92.94 years and are roughly as far apart from each other as the Sun and Neptune. The brighter component has been classed as a Delta Scuti variable star, though this view is not universal. The components are main sequence stars of spectral types B9V and A3V. Located 170±2 light-years away, 4.06-magnitude Delta Coronae Borealis is a yellow giant star of spectral type G3.5III that is around and has swollen to .

Beta Carinae, traditionally called Miaplacidus, is a blue-white hued star of magnitude 1.7, 111 light-years from Earth. Epsilon Carinae is an orange-hued giant star similarly bright to Miaplacidus at magnitude 1.9; it is 630 light-years from Earth. Another fairly bright star is the blue-white hued Theta Carinae; it is a magnitude 2.7 star 440 light-years from Earth. Theta Carinae is also the most prominent member of the cluster IC 2602. Iota Carinae is a white-hued supergiant star of magnitude 2.2, 690 light-years from Earth.

Kappa Crateris (κ Crateris) is the Bayer designation for a star in the southern constellation of Crater. It has an apparent visual magnitude of 5.94, which, according to the Bortle scale, can be seen with the naked eye under dark suburban skies. The distance to this star, as determined from an annual parallax shift of 14.27 mas, is around 229 light years. This is an evolved F-type giant star with a stellar classification of F5/6 III, where the F5/6 indicates the spectrum lies intermediate between types F5 and F6.

The visible component is an aging red giant star on the asymptotic giant branch with a stellar classification of M1III, indicating it has exhausted the supply of both hydrogen and helium at its core and is cooling and expanding. It is a suspected variable star of unknown type that has been measured ranging in brightness from visual magnitude 4.94 down to 5.07. At present it has 48 times the radius of the Sun. It is radiating 502 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,948 K.

These stars represent a late stage in the evolution of some stars, caused when a red giant star loses its outer hydrogen layers before the core begins to fuse helium. The reasons why this premature mass loss occurs are unclear, but the interaction of stars in a binary star system is thought to be one of the main mechanisms. Single subdwarfs may be the result of a merger of two white dwarfs. The sdB stars are expected to become white dwarfs without going through any more giant stages.

Gamma Hydrae (γ Hya, γ Hydrae) is a star in the equatorial constellation of Hydra. It has an apparent visual magnitude of 3.0, placing it second in brightness among the members of this generally faint constellation. Based upon parallax measurements made during the Hipparcos mission, this star is at a distance of around from Earth. The stellar spectrum matches a stellar classification of G8 III, with the luminosity class of III indicating it has evolved into a giant star after exhausting the supply of hydrogen at its core.

This object is an aging G-type giant star with a stellar classification of G8III. Having exhausted the supply of hydrogen at its core, it has expanded and cooled off the main sequence; at present it has 6.5 times the girth of the Sun. The star has 1.6 times the mass of the Sun and is radiating 24 times the Sun's luminosity from its swollen photosphere at an effective temperature of 5008 K. These coordinates are a source for X-ray emission, which is most likely (99.3% chance) coming from the star.

Pi Hydrae (π Hya, π Hydrae) is a star in the constellation Hydra with an apparent visual magnitude of 3.3, making it visible to the naked eye. Parallax measurements put this star at a distance of about from the Earth. The spectrum of this star shows it to have a stellar classification of K1 III-IV, with the luminosity class of 'III-IV' suggesting it is in an evolutionary transition stage somewhere between a subgiant and a giant star. It has a low projected rotational velocity of 2.25 km s−1.

HD 173416 b is an extrasolar planet located approximately 440 light years away in the constellation of Lyra, orbiting the 6th magnitude G-type giant star HD 173416. This is planet has at least 2.7 times the mass of Jupiter and was discovered on January 10, 2009 by Liu et al. HD 173416 b orbits at 1.16 AU from the star. However, despite the fact that the planet orbits 16% further from the star than Earth does from the Sun, it has orbital period of only 323.6 days, compared to 365.25 days for Earth.

The primary, component A, is an evolved, K-type giant star with a stellar classification of K3 IIIb. It is a weak barium star, indicating that the atmosphere was previously enriched by accretion of s-process elements from what is now a white dwarf companion. The giant has 1.66 times the mass of the Sun and has expanded to about 34 times the Sun's radius. It is about 3.4 billion years old and is radiating 380 times the Sun's luminosity from its photosphere at an effective temperature of 4,154 K.

The mass of L 97-12 is 0.59 ± 0.01 Solar masses, and its surface gravity is 108.00 ± 0.02 cm·s−2, or approximately 102,000 of Earth's, corresponding to a radius of , or 139% of Earth's. L 97-12 has temperature 5,700 ± 90 K, almost like the Sun, and cooling age, i.e. age as degenerate star (not including lifetime as main- sequence star and as giant star) 2.65 ± 0.10 Gyr. Despite it is classified as "white dwarf", it should appear yellow, not white, nearly the same color as the Sun.

Discovery of the binary nature of this system is credited to Canadian astronomer H. H. Plaskett in 1922. It is a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.24. The visible component is an aging giant star with a stellar classification of G9 III, having exhausted the supply of hydrogen at its core and expanded to 10.7 times the Sun's radius. It is a red clump giant, indicating it is on the horizontal branch and is generating energy via core helium fusion.

This is an evolved bright giant star with a stellar classification of F7/8 II. The spectrum displays a deficit of carbon, an excesses of nitrogen, and a high abundance of lithium. The first two anomalies suggest the giant has passed through a deep convection stage that would have also exhausted the lithium supply, indicating the current lithium abundance is of recent production. The star has 2.7 times the mass of the Sun and is radiating 515 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,868 K.

Xi2 Ceti (ξ2 Ceti) is a star located in the constellation Cetus, approximately 60 parsecs from Earth. Xi2 Ceti is a spectrophotometric standard star. It has exhausted its core hydrogen, evolved away from the main sequence, and expanded to become a giant star, although still only 127 million years old. In Chinese, (), meaning Circular Celestial Granary, refers to an asterism consisting of α Ceti, κ1 Ceti, λ Ceti, μ Ceti, ξ1 Ceti, ξ2 Ceti, ν Ceti, γ Ceti, δ Ceti, 75 Ceti, 70 Ceti, 63 Ceti and 66 Ceti.

G 240-72 has mass 0.81 Solar masses and surface gravity 108.36 (2.29 · 108) cm·s−2, or approximately 234 000 of Earth's, corresponding to a radius 6850 km, or 107% of Earth's. This white dwarf has relatively low temperature 5590 K (slightly cooler than the Sun), and old cooling age, i. e. age as degenerate star (not counting duration of previous existence as main sequence star and as giant star) 5.69 Gyr. Despite being classified as "white dwarf", it should appear yellow, not white, due to low temperature.

WD 2359−434's mass is 0.85 ± 0.01 Solar masses, its surface gravity is 108.39 ± 0.01 (2.45 · 108) cm·s−2, or approximately 250,000 of Earth's, corresponding to a radius 6780 km, or 1.06 of Earth's. WD 2359−434 is relatively hot and young white dwarf, its temperature is 8570 ± 50 K; its cooling age, i. e. age as degenerate star (not including lifetime as main sequence star and as giant star) is 1.82 ± 0.06 Gyr. Gliese 518 should appear bluish-white, due temperature, comparable with that of A-type main sequence stars.

NGC 6940 has hundreds of members. The cluster is quite scattered and in between its members are also visible field stars. For example, two bright stars, an 8.6 mag B8III giant star at the NE edge and a 9.1 mag A0III giant at the SW corner of the cluster are too young to be true members of NGC 6940 and are probably background stars. The brightest star (lucida) of NGC 6940 is the red giant VG Vulpeculae, a semiregular variable star whose magnitude ranges from 9.0 to 9.5 every 80 days approximately.

It is actually a confirmed spectroscopic binary system with a high temperature subdwarf O-type companion in a 28-day orbital period. The latter is heating the nearest side of the circumstellar gaseous disk that surrounds the primary. Orbiting the primary pair is 59 Cyg Ab, a magnitude 7.64 A-type main-sequence star of class A3V, located at an angular separation of . A fourth component is a magnitude 9.8 A-type giant star of class A8III at a separation of along a position angle (PA) of 352°, as of 2008.

This is an aging giant star with a stellar classification of , where the suffix notation indicates a mild underabundance of iron in the spectrum. It has 1.7 times the mass of the Sun but has expanded to 14 times the Sun's radius. The star is radiating 69 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,640 K. 72 Cygni has a wide companion at an angular separation of , corresponding to a projected separation of . This star has a J band (infrared) magnitude of and a class of M5.

This is a K-type giant star with a stellar classification of K2 III:, where the semi-colon indicates some uncertainty about its spectral value. It is considered metal- rich star and is past the first dredge-up phase of its post-main sequence evolution, although it shows under-abundances of carbon and oxygen in its spectrum. The star has 1.25 times the mass of the Sun and is an estimated 6.48 billion years old. It is radiating 48 times the solar luminosity from its enlarged photosphere at an effective temperature of 4,413 K.

33 Vulpeculae is a single star located around 500 light years away from the Sun in the northern constellation of Vulpecula. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.31. The object is drifting closer to the Earth with a heliocentric radial velocity of −25 km/s. This is an evolved giant star with a stellar classification of K3.5 III, having exhausted the supply of hydrogen at it its core and expanded to 35 times the Sun's radius.

This is an aging K-type giant star with a stellar classification of K0III, having exhausted the supply of hydrogen at its core and expanded to 11 times the Sun's radius. It is a red clump giant, which indicates it is on the horizontal branch and is generating energy from core helium fusion. The star is now 2.5 billion years old with 1.6 times the mass of the Sun. It is radiating 60 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,825 K.

According to Ken Beck and Jim Clark, Bruno and a brother were orphaned in Wisconsin as cubs, and later acquired by Helfer from a private party. It was reported during the Gentle Ben series run that Bruno (who at that point had been renamed "Ben" for the run of the show"'Gentle Giant' Star Changes Name For Marquee Lure", Daily Republican (Monongahela, Penn.), Feb. 16, 1968, p. 10.) had been "discovered" in White Lake, Wisconsin, and that he was 6 years old in 1968, making his birth year 1962.

This is a giant star with a stellar classification of K2.5III, indicating that this star has consumed the hydrogen at its core and has evolved away from the main sequence. It has expanded to an estimated radius of about 48 times the radius of the Sun and is emitting 980 times the Sun's luminosity. The photosphere has an effective temperature of 4,256 K, giving the star the characteristic orange hue of a K-type star. Based upon parallax measurements, this star is 430 ± 20 light-years from the Earth.

The novel takes place on the planet of Worlorn, a world which is dying. It is a rogue planet whose erratic course is taking it irreversibly away from its neighboring stars into a region of cold and dark space where no life will survive. Worlorn's 14 cities, built during a brief window when the world passed close enough to a red giant star to permit life to thrive, are dying, too. Constructed to celebrate the diverse cultures of 14 planetary systems, they have largely been abandoned, allowing their systems and maintenance to fail.

The star is moving further from the Sun with a heliocentric radial velocity of +16 km/s. The stellar classification of 75 Tauri is K1 IIIb, indicating it is an aging giant star that has exhausted the supply of hydrogen at its core. At the estimated age of roughly 2.7 billion years, this has become a red clump star that is generating energy through helium fusion in its core region. The star has 1.5 times the mass of the Sun and has expanded to 11 times the Sun's radius.

The primary member of this system, component A, is an evolved red giant star, currently on the asymptotic giant branch, with a stellar classification of M2− IIIab. It is a suspected variable star of unknown type with a brightness that varies from visual magnitude 4.95 down to 5.00. As of 2011, the magnitude 9.88 secondary, component B, lay at an angular separation of along a position angle of 226° relative to the primary. In the sky, the open cluster Messier 52 is 40' to the south of it, near the constellation border with Cepheus.

As of 2016, the secondary had an angular separation of along a position angle of 165° from the primary. They are moving further from the Earth with a heliocentric radial velocity of +7 km/s. The brighter star, designated component A, is a magnitude 6.40 giant star with a stellar classification of K1 III. The companion star, component B, is a magnitude 7.20 A-type main sequence star with a classification of A6 V. Helmut Abt (1985) had this star classified as A3 IV, matching a more evolved subgiant.

The star is moving closer to the Earth with a heliocentric radial velocity of −4.7 km/s. The spectrum of this object is that of a subgiant star with a stellar classification of G7 IV, which would suggest it has exhausted the supply of hydrogen at its core and has begun to evolve into a giant star. It is around 1.7 billion years old with a projected rotational velocity of 1.8 km/s. The star has nearly double the mass of the Sun and almost six times the Sun's radius.

Because this star is positioned near the ecliptic, it is subject to lunar eclipses. This object is an aging red giant star currently on the asymptotic giant branch with a stellar classification of M2 III, having exhausted both the hydrogen and helium at its core and expanded to 56 times the Sun's radius. It is a suspected variable star of unknown type that ranges in magnitude between 6.24 and 6.29. The star is radiating 693 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3,946 K.

It is receding from the Earth with a heliocentric radial velocity of +24 km/s. This object is an aging giant star with a stellar classification of K3 III, having exhausted the supply of hydrogen at its core and expanded to 11 times the Sun's radius. It is 5.3 billion years old with 1.36 times the mass of the Sun. The star shines with 49 times the Sun's luminosity; this energy is being radiated from the photosphere at an effective temperature of 4,449 K, giving it the orange-hued glow of a K-type star.

This has been identified as a visual binary system with an orbital period of in a circular orbit (eccentricity of zero). The primary component has a stellar classification of A9/F0 V, matching a main sequence star with a spectrum showing mixed traits of an A/F-type. (Cowley and Fraquelli [1974] has previously assigned it a giant star class of A8 III.) It is a chemically peculiar Am star, showing metallic lines with no magnetic field. The star has 1.7 times the mass of the Sun and 2.1 times the Sun's radius.

The star is moving closer to the Earth with a heliocentric radial velocity of −22.5 km/s. The stellar classification of 69 Aquilae is K1/2 III, which means this is an evolved giant star. It belongs to a sub-category called the red clump, indicating that it is on the horizontal branch and is generating energy through helium fusion at its core. The star is about 3.4 billion years old with 1.54 times the mass of the Sun and has expanded to 11 times the Sun's radius.

The spectrum of this star matches a stellar classification of M1 III. It is a red giant star with 54 times the radius of the Sun that is currently on the asymptotic giant branch. This means the star is generating energy by the fusion of hydrogen along an outer shell and helium along a concentric inner shell, surrounding an inert core of carbon and oxygen. 36 Aquilae undergoes small, periodic variations in luminosity, changing by 0.0063 magnitudes about 11.5 times per day, or once every 2 hours and 5.2 minutes.

At the age of 2.72 billion years, this is an evolved G-type giant star with a stellar classification of G8.5 III. It belongs to the so-called "red clump", which indicates it is generating energy through helium fusion at its core. Although it displays a higher abundance of barium than is normal for a star of its type, Williams (1975) considers its status as a Barium star to be "very doubtful". The star has double the mass of the Sun and has expanded to 11 times the Sun's radius.

The visible component is an aging giant star with a stellar classification of . The suffix notation indicates this is a mild barium star, which means the stellar atmosphere is enriched with s-process elements. It is either a member of a close binary system and has previously acquired these elements from a (now) white dwarf companion or else it is on the asymptotic giant branch and is generating the elements itself. 2 Aurigae is 1.80 billion years old with 2.86 times the mass of the Sun and has expanded to 48 times the Sun's radius.

The star is moving closer to the Earth with a heliocentric radial velocity of −5 km/s. This is a mildly iron-deficient giant star with a stellar classification of K4.5 III, which indicates that, at the age of three billion years, is an evolved star that has exhausted the hydrogen at its core and expanded its radius. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of this star, this yields a physical size of about 47 times the radius of the Sun.

The measured annual parallax shift of 27.52 mas is equivalent to a distance of approximately from Earth. The spectrum of this star matches a stellar classification of A7 III-IV, with the luminosity class of III-IV indicating it shows traits part way between the subgiant and giant star stages of its evolution. It is a Delta Scuti variable with a period of 0.0355 days (51 minutes) and a magnitude change of 0.040. This star is larger than the Sun, with more than double the Sun's radius and 11 times the luminosity.

A stellar classification of G6 III indicates this is an evolved giant star, most likely (98% chance) on the horizontal branch, having exhausted the hydrogen at its core and expanded. It is a suspected variable star of unknown type. 44 Aquarii is 537 million years old with about 2.53 times the mass of the Sun and 9 times the Sun's radius. The star is radiating 62 times the Sun's luminosity from its photosphere at an effective temperature of 5,025 K. At this heat, the star has the golden-hued glow of a G-type star.

This star is 3.79 billion years old with a stellar classification of G8 III, indicating the is a giant star that has exhausted the hydrogen at its core and expanded off the main sequence. It is a red clump giant, which means it is on the horizontal branch and is generating energy through helium fusion at its core. It has 1.39 times the mass of the Sun and 10 times the Sun's radius. The star is radiating 59 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 5,036 K.

The spectrum of this star matches a stellar classification of B1.5 IV, which indicates this star has entered the subgiant stage and is in the process of evolving into a giant star. It is radiating around 10,000 times the luminosity of the Sun from its outer atmosphere at an effective temperature of 23,000 K, giving it a blue-white hue. This star has nearly 12 times the mass of the Sun and is roughly 15 million years old. Delta Lupi is a Beta Cephei variable star that undergoes periodic pulsations.

It is moving closer to the Earth with a heliocentric radial velocity of −5 km/s. With an age of 420 million years, this is a red giant star with a stellar classification of G8 III, indicating it has consumed the hydrogen at its core and evolved off the main sequence. It has 2.8 times the mass of the Sun and has expanded to 12 times the Sun's radius. The star is radiating 90 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,107 K.

It is moving further from the Earth with a heliocentric radial velocity of +10 km/s. This is an evolved giant star with a stellar classification of K0 III, which means it has exhausted the supply of hydrogen at its core and turned off the main sequence. It has an estimated 2.57 times the mass of the Sun and has expanded to around 12 times the Sun's radius. It is radiating 63 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,874 km/s.

Gamma Lupi (γ Lupi, γ Lup) is a 3rd-magnitude, B-type blue giant star in the constellation of Lupus. It is also known in ancient Chinese astronomy as 騎官一 or "the 1st (star) of the Cavalry Officer". With a telescope, Gamma Lupi can be resolved into a binary star system in close orbit. This is known as the Gamma Lupi AB system, often abbreviated as γ Lupi AB or γ Lup AB. Gamma Lupi A is itself a spectroscopic binary with a period of 2.8081 days.

Omega Boötis (ω Boötis) is the Bayer designation for a solitary, orange-hued star in the northern constellation of Boötes. It is a dim star but visible to the naked eye with an apparent visual magnitude of +4.82. Based upon an annual parallax shift of 8.78 mas as seen from the Earth, it is located about 370 light years from the Sun. This star is three billion years old with a stellar classification of K4 III, matching an evolved K-type giant star that has consume the supply of hydrogen at its core.

2 Boötis is a single star in the northern constellation of Boötes, located 337 light years away from the Sun. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 5.63. This object is moving further from the Earth with a heliocentric radial velocity of +4 km/s. At the age of 1.33 billion years old, this is an evolved giant star with a stellar classification of K0 III, having exhausted the hydrogen at its core and expanded off the main sequence.

With a stellar classification of A5 III, this appears to be an evolved, A-type giant star. At the age of about 600 million years, it has double the mass of the Sun and 1.86 times the Sun's radius. Omicron1 Cancri is radiating 13.4 times the solar luminosity from its photosphere at an effective temperature of about 8,636 K. Omicron1 Cancri has an infrared excess, indicating it surrounded by a circumstellar debris disk. The signature matches a two-component disk with the spatially-separated belts having temperatures of 146 K and 81 K.

The primary, designated component A, is K-type giant star with a stellar classification of K5 III, having exhausted the supply of hydrogen at its core, then cooled and expanded. At present it has 40 times the girth of the Sun. It is radiating 353 times the luminosity of the Sun at an effective temperature of 3,955 K. In Chinese astronomy, Ghost () refers to an asterism consisting of Theta Cancri, Eta Cancri, Gamma Cancri and Delta Cancri. Theta Cancri is the first star of Ghost (), as it is also the determinative star for that asterism.

9 Boötis is a single, variable star in the northern constellation of Boötes, located around 630 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with a baseline apparent visual magnitude of 5.02. This object is moving closer to the Earth with a heliocentric radial velocity of −41 km/s. This is an aging giant star with a stellar classification of K3 III, which indicates it has exhausted the hydrogen at its core and evolved of the main sequence.

39 Arietis (Lilii Borea) is an orange giant star of magnitude 4.51 and spectral type K1.5III that is around 171 light-years distant. The constellation was renamed Vespa by Jakob Bartsch in 1624. The renaming by Bartsch may have been intended to avoid confusion with another constellation, created by Plancius in 1598, that was called Apis by Bayer in 1603. Plancius called this earlier constellation Muia (Greek for fly) in 1612, and it had been called Musca (Latin for fly) by Blaeu in 1602, although Bayer was evidently unaware of this.

Beta Pavonis is a member of the Ursa Major Moving Group, a set of stars that share a similar motion through space. Zorec and Royer (2012) list a stellar classification for this star of A5 IV, indicating it is an evolving subgiant star that has consumed the hydrogen at its core and has begun to expand onto the red giant branch. However, Houk (1979) listed a more evolved class of A7 III, suggesting it is already a giant star. It has about 2.3 times the Sun's radius and 2.51 times the mass of the Sun.

This is an evolved red giant star with a stellar classification of M0 III. It is estimated to have 1.52 times the mass of the Sun, but has expanded to 44 times the Sun's radius. The star is spinning with a projected rotational velocity of 5.9 km/s and is about 3.53 billion years old. Upsilon Geminorum is radiating 417 times the solar luminosity from its outer atmosphere at an effective temperature of 3926 K. Based upon the motion of this star through space, Upsilon Geminorum is a member of the Wolf 630 moving group.

45 Eridani is a single star located around 700 light years away from the Sun in the equatorial constellation of Eridanus. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.91. This body is moving away from the Earth with a heliocentric radial velocity of +15 km/s. The stellar classification for this star is K0/1 III, which indicates this is an aging K-type giant star that has exhausted the hydrogen supply at its core and expanded.

Pismis 24-1 has been resolved visually into two components, usually labelled as NE and SW from their orientation with each other. Pismis 24-1NE is slightly more luminous and hotter than 24-1SW, but is known to be a spectroscopic binary. This is surprising given the spectral luminosity classes, because it would make the individual supergiant stars less luminous than a single cooler giant star. It could be that the interaction between the components of 24-1NE is confusing its classification, or the O4 giant may also be a close binary.

The visible component has a stellar classification of , indicating it is an evolved K-type giant star with some abundance peculiarities in its atmosphere. At the age of around 280 million years, it is most likely (99% chance) on the horizontal branch. It is a barium star, which suggests it may have a degenerate white dwarf companion from which it accreted materials during an earlier stage of its evolution. 18 Dra has an estimated 3.8 times the mass of the Sun and has expanded to 47 times the Sun's radius.

The luminosity class of 'III' indicates this is a giant star that has exhausted the hydrogen at its core and evolved away from the main sequence. It is radiating energy from its outer atmosphere at an effective temperature of 4,246 K which is what gives it the orange hue of a K-type star. This star displays an excess of infrared emission that may indicate circumstellar matter. In Chinese, (), meaning Tortoise, refers to an asterism consisting of ζ Arae, ε1 Arae, γ Arae, δ Arae and η Arae.

This is an aging red giant star on the asymptotic giant branch with a stellar classification of M1 III, a star that has exhausted the supply of hydrogen at its core then cooled and expanded. At present it has 76 times the radius of the Sun. It is a suspected variable star of unknown type with a brightness that has been measured ranging from a peak of 5.19 down to 5.24. The star is radiating 1,283 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3,953 K.

It is drifting further away from the Sun with a radial velocity of about +27 km/s. The system is a member of the Vel OB2 association of co-moving stars. The double nature of this system was discovered in 1896 by Scottish astronomer Robert T. A. Innes – it is now known to be a double-lined spectroscopic binary. The magnitude 5.14 primary component has a blue-white hue and has been assigned stellar classifications of B1V and B2III, matching a B-type main-sequence star or a giant star, respectively.

This is an aging giant star with a stellar classification of K4III, having exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. It now has 22 times the girth of the Sun and is radiating 151 times the luminosity of the Sun at an effective temperature of 4,304 K. The metallicity, or abundance of elements with higher atomic numbers than helium, is lower than in the Sun, and it is spinning slowly with a projected rotational velocity of 1.0 km/s.

This is an aging giant star with a stellar classification of K5III. Having exhausted the supply of hydrogen at its core, it has cooled and expanded off the main sequence and now has 51 times the girth of the Sun. It is classified as a probable semiregular variable star with a sub-type of SRd and a brightness that varies from visual magnitude 5.66 down to 5.86 over a period of 56.5 days. The star is an estimated 2.85 billion years old with 1.73 times the mass of the Sun.

This is an aging giant star with a stellar classification of K0III, having evolving off the main sequence after the supply of hydrogen at its core was exhausted. It is an estimated 4.78 billion years old with 1.39 times the mass of the Sun, although Bailer-Jones et al. (2018) give a higher estimate of 2.8 times the Sun's mass. The elemental composition of this star has made it the first giant to be a candidate solar sibling, suggesting it may have been born in the same star cluster as the Sun.

It has 12 times the mass of the Sun and has expanded to 202 times the Sun's radius. The star is radiating 8,478 times the luminosity of the Sun from its bloated photosphere at an effective temperature of 3,900 K. The magnitude 7.48 companion star, component B, was discovered by J. Dunlop in 1829. As of 2015, it was located at an angular separation of along a position angle of 21°, relative to the primary. It is a B-type giant/bright giant star with a class of B9II/III.

Omega Carinae has a stellar classification of B8 IIIe, which places it in the category of Be stars, that display emission lines of hydrogen their spectrum. Omega Carinae is a shell star, having a circumstellar disk of gas surrounding its equator. The luminosity class of III indicates it has evolved into a giant star, having exhausted the hydrogen at its core and left the main sequence. The effective temperature of in its outer envelope is what gives this star the blue-white hue that is characteristic of B-type stars.

Alpha Doradus (Alpha Dor, α Doradus, α Dor) is the brightest star in the southern constellation of Dorado. The distance to this system, as measured using the parallax method, is about . This is a binary star system with an overall apparent visual magnitude that varies between 3.26 and 3.30, making this one of the brightest binary stars. The system consists of a subgiant star of spectral type B revolving around a giant star with spectral type A in an eccentric orbit with a period of about 12 years.

The primary component of this system has a stellar classification of K1 III. A luminosity class 'III' indicates this has expanded into a giant star after exhausting the supply of hydrogen at its core and evolving away from the main sequence of stars like the Sun. The interferometry-measured angular diameter of this star, after correcting for limb darkening, is , which, at its estimated distance, equates to a physical radius of about 27 times the radius of the Sun. It appears to be rotating slowly, with a projected rotational velocity of .

Artist's impression of a low-mass X-ray binary (LMXB): an evolved low-mass yellow sub-giant star transfers mass to a neutron star. Because the accretor is a compact object, an accretion disc forms, which is the source of the X-rays. Source. An Interacting binary star is a type of binary star in which one or both of the component stars has filled or exceeded its Roche lobe. When this happens, material from one star (the donor star) will flow towards the other star (the accretor).

This object is an A-type giant star with a stellar classification of A2IIIshe. The suffix notation indicates this is a shell star, which means it has a peculiar spectrum indicating there is a circumstellar disk of gas around the star's equator. While the spectral luminosity class is III, analysis of its colour and brightness suggest it more closely resembles a supergiant star. HD 32188 has expanded to 30 times the radius of the Sun and it is spinning with a projected rotational velocity of 23 km/s.

This was found to be a double star by R. A. Rossiter in 1953, with the magnitude 13.7 companion having an angular separation of along a position angle of 266°, as of 2016. The brighter, magnitude 4.32 component A is a spectroscopic binary. As of 2009, the orbital solution for this pair is of low quality, giving a period of roughly and an eccentricity of around 0.4. The primary component is an aging giant star with a stellar classification of , where the suffix notation indicates an underabundance of the cyanogen molecule.

This is an F-type subgiant star with a stellar classification of F8 IVw, which indicates it has nearly consumed the hydrogen at its core and is now evolving into a giant star. It is a low amplitude Delta Scuti variable that varies by 0.02 magnitude. At the age of 1.7 billion years it is spinning with a projected rotational velocity of 5.7 km/s. The star has 1.77 times the mass of the Sun and is radiating 12 times the Sun's luminosity from its photosphere at an effective temperature of 6,276 K.

Tau1 Serpentis, Latinized from τ1 Serpentis, is a single star in the Caput (Head) segment of the equatorial constellation of Serpens. It is a red hued star that is dimly visible to the naked eye with an apparent visual magnitude of 5.16. Based upon parallax measurements, this star is located at a distance of approximately 990 light years from the Sun, while it is drifting closer with a radial velocity of −16.5 km/s. This object is an aging red giant star, currently on the asymptotic giant branch, with a stellar classification of M1III.

42 Draconis (abbreviated 42 Dra), formally named Fafnir ( or ), is a 5th magnitude K-type giant star located approximately 315 light years away in the constellation of Draco. As of 2009, an extrasolar planet (designated 42 Draconis b, later named Orbitar) is thought to be orbiting the star. Of spectral type K1.5III, the star has a mass similar to the Sun but with a radius 22 times greater. It is a metal-poor star with metallicity as low as 35% that of the Sun and its age is 9.49 billion years.

This is an aging giant star with a class of K3, which has exhausted the supply of hydrogen at its core and expanded to 25 times the radius of the Sun. It is around three billion years old with 1.3 times the Sun's mass. The star is radiating 152 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,019 K. It is spinning slowly, with each rotation taking at least . On June 10, 2009 a planet orbiting the star was discovered by Niedzielski et al.

Once an A-type main sequence star, Pollux has exhausted the hydrogen at its core and evolved into a giant star with a stellar classification of K0 III. The effective temperature of this star's outer envelope is about , which lies in the range that produces the characteristic orange hue of K-type stars. Pollux has a projected rotational velocity of . The abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, is uncertain, with estimates ranging from 85% to 155% of the Sun's abundance.

This object has a stellar classification of B9.5 III, matching a giant star that has consumed the hydrogen at its core and is evolving away from the main sequence. It is spinning rapidly with a projected rotational velocity of 246 km/s, compared to a critical velocity of 270 km/s. The star has 4.5 times the mass of the Sun and about 3.6 times the Sun's radius. It is radiating around 1,000 times the luminosity of the Sun from its photosphere at an effective temperature of 10,471 K.

2 Piscis Austrini, also known as HR 8076, is a single star located approximately 351 light years away in the southern constellation of Microscopium, despite its Flamsteed designation. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.2. This is an aging giant star with a stellar classification of K3 III. At the age of 2 billion years, it is a red clump giant, which indicates it is on the horizontal branch and is generating energy through helium fusion at its core.

Examination of this star's spectrum show it to match a stellar classification of G9 III, with the 'III' luminosity class revealing that it has consumed the hydrogen fuel at its core and expanded into the giant star stage of its stellar evolution. It is known to vary in luminosity, but only by about 0.01 to 0.02 magnitudes. The measured angular diameter of this star, after correction for limb darkening, is . At an estimated distance of based on parallax measurements, this yields a physical size of about 8–9 times the radius of the Sun.

Omicron Draconis (Latinised as ο Draconis, abbreviated to ο Dra) is a giant star in the constellation Draco located 322.93 light years from the Earth. It has a radius of 30 solar radii, and a luminosity of 269 suns. Its path in the night sky is circumpolar above the ecliptic, meaning the star never rises or sets when viewed in the night sky from certain positions in the northern hemisphere. Omicron Draconis can be considered the north pole star of Mercury, as it is the closest star to Mercury's north celestial pole.

HD 222093 is a double star in the equatorial constellation of Aquarius. It has an orange hue and is visible to the naked eye with an apparent visual magnitude of 5.68. The system is located at a distance of approximately 293 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −13 km/s. The primary component is an aging K-type giant star with a stellar classification of K0III, which indicates it has exhausted the supply of hydrogen at its core then cooled and expanded.

Last to join on pedal steel was Chris Funk of The Decemberists, who, upon hearing the band's early demos, demanded to join the band. Infused with their own respective indie-rock, punk and DIY backgrounds, the Blue Giant songs reflect a greater part of the Robinson's Southern heritage. The band name is a reference to a blue giant star, a transitory phase in the life cycle of a star, and one of the brightest types of stars in the universe. Blue Giant played their first show in June 2008 headlining the Wonder Ballroom in Portland.

Algol B Bellatrix is a massive star with about 8.6 times the Sun's mass. It has an estimated age of approximately 25 million years—old enough for a star of this mass to consume the hydrogen at its core and begin to evolve away from the main sequence into a giant star. The effective temperature of the outer envelope of this star is , which is considerably hotter than the 5,778 K on the Sun. This high temperature gives this star the blue-white hue that occurs with B-type stars.

Epsilon Draconis is a yellow giant star with a spectral type of G8III. It has a radius that has been estimated at 10 solar radii and a mass of 2.7 solar masses. Compared to most G class stars, Epsilon Draconis is a relatively young star with an estimated age of around 500 million years old. Like the majority of giant stars, Epsilon Draconis rotates slowly on its axis with a rotational velocity of 1.2 km/s, a speed which takes the star approximately 420 days to make one complete revolution.

It was first resolved by Harold A. McAlister (1978), who found an angular separation of along a position angle of The magnitude 7.24 primary component is an evolved giant star with a stellar classification of G8/K0 III, indicating it has exhausted the hydrogen at its core and expanded off the main sequence. It is radiating 73 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,700 K. The companion is a hot A-type star of uncertain luminosity class, with a visual magnitude of 8.89.

18 Sagittarii is a single star in zodiac constellation of Sagittarius, located around 550 light years away from the Sun based on parallax. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.58. This object is moving closer to the Earth with a heliocentric radial velocity of −19 km/s. This is an aging giant star with a stellar classification of K0 III, which indicates it has exhausted the hydrogen at its core and evolved away from the main sequence.

HD 104985 b, also named Meztli , is an extrasolar planet approximately 97 parsecs (317 lys) from the SunThe 198-day period planet orbits the yellow giant star HD 104985 (Tonatiuh) at a distance of 0.78 AU. With a mass 61/3 times Jupiter it is a gas giant. Following its discovery in 2003 the planet was designated HD 104985 b. In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars.NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org.

This is an evolving B-type star with a stellar classification of B4 IV/V, having a luminosity class intermediate between a subgiant and a giant star. It has an estimated five times the mass of the Sun and 3.4 times the Sun's radius. Kappa Hydrae has a high rate of spin with a projected rotational velocity of 115.0 km/s, and is only about 31 million years old. The star radiates 328 times the solar luminosity from its outer atmosphere at an effective temperature of 16,150 K.

Subdwarf B stars such as V391 Pegasi are thought to be the result of the ejection of the hydrogen envelope of a red giant star at or just before the onset of helium fusion. The ejection left only a tiny amount of hydrogen on the surface—less than 1/1000 of the total stellar mass. The future for the star is to eventually cool down to make a low-mass white dwarf. Most stars retain more of their hydrogen after the first red giant phase, and eventually become asymptotic giant branch stars.

36 Persei is a solitary, variable star located 121 light years away from the Sun in the northern constellation of Perseus. It is visible to the naked eye as a dim, yellow-white hued point of light with a baseline apparent visual magnitude of 5.32. The star is drifting closer to the Sun with a heliocentric radial velocity of −47.5 km/s, and may come as close as in 661,000 years. The stellar classification of 36 Persei is F4III, matching an aging giant star that has used up its core hydrogen.

Nu1 Lupi (ν1 Lup) is a solitary star in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 5.01. It is a high proper motion star with an annual parallax shift of 27.89 mas as seen from Earth, yielding a distance estimate of 117 light years from the Sun. This is a two billion year old evolved star with a stellar classification of F6 III-IV, indicating that the spectrum has characteristics intermediate between a subgiant and giant star.

The visible-light (left) and infrared (right) views of the Trifid Nebula, a giant star-forming cloud of gas and dust located away in the constellation Sagittarius Stars are thought to form inside giant clouds of cold molecular hydrogen—giant molecular clouds of roughly and in diameter. Over millions of years, giant molecular clouds are prone to collapse and fragmentation. These fragments then form small, dense cores, which in turn collapse into stars. The cores range in mass from a fraction to several times that of the Sun and are called protostellar (protosolar) nebulae.

Epsilon Tauri b (abbreviated ε Tauri b or ε Tau b), formally named Amateru , is a super-Jupiter exoplanet orbiting the K-type giant star Epsilon Tauri approximately 155 light-years (47.53 parsecs, or nearly km) away from the Earth in the constellation of Taurus. It orbits the star further out than Earth orbits the Sun. It has moderate eccentricity. The planet orbits one of the four giant stars in the Hyades cluster that is 2.7 times the mass of our Sun, making it the most massive planet-harboring star.

A view of Alpha Herculis in a small telescope. The components A and B are resolved with angular separation of 4.64 (in 2020). Alpha Herculis A and B are more than 500 AU apart, with an estimated orbital period of approximately 3600 years. A presents as a relatively massive red bright giant, but radial velocity measurements suggest a companion with a period of the order of a decade. B's two components are a primary yellow giant star and a secondary, yellow-white dwarf star in a 51.578 day orbit.

Individual spectral types for the two components are difficult to assign accurately, especially for the secondary due to the Struve–Sahade effect. The Bright Star Catalogue derived a spectral class of B1 III-IV for the primary and B2V for the secondary, but later studies have given various different values. The primary star has a stellar classification of B1 III–IV. The luminosity class matches the spectrum of a star that is midway between a subgiant and a giant star, and it is no longer a main-sequence star.

The spectrum of this massive star matches a stellar classification of B0.5 IVe. A luminosity class of IV identifies it as a subgiant star that has reached a stage of its evolution where it is exhausting the supply of hydrogen in its core region and transforming into a giant star. The 'e' suffix is used for stars that show emission lines of hydrogen in the spectrum, caused in this case by the circumstellar disk. This places it among a category known as Be stars; in fact, the first such star ever to be so designated.

This is a red giant star on the asymptotic giant branch with an estimated mass of about 2.4 times that of the Sun and a surface temperature of approximately 3,480 K, just over half the surface temperature of the Sun. This low temperature accounts for the dull red color of an M-type star. The total luminosity is about 2,500 times that of the Sun, and it has estimated 180 times the Sun's radius. Beta Gruis is a semiregular variable (SRb) star that varies in magnitude by about 0.4.

The primary star has a stellar classification of G7 IIIa, indicating that it is a giant star that has exhausted the hydrogen at its core and evolved away from the main sequence. It has a mass nearly three times the mass of the Sun, and has expanded to 17 times the Sun's radius. The effective temperature of the star's outer envelope is about 4,887 K, which gives it the yellow hue of a G-type star. The secondary star has a mass only 90% that of the Sun.

Epsilon Ophiuchi (ε Ophiuchi, abbreviated Epsilon Oph, ε Oph), formally named Yed Posterior , is a red giant star in the constellation of Ophiuchus. Located less than five degrees south of the celestial equator in the eastern part of the constellation, it forms a naked eye optical double with Delta Ophiuchi (named Yed Prior). With an apparent visual magnitude of 3.220, the star can be seen with the naked eye from most of the Earth under suitably dark skies. Parallax measurements yield an estimated distance of from the Sun.

Epsilon Ophiuchi has a stellar classification of G9.5 IIIb, with the luminosity class of III indicating that this is a giant star that has exhausted the hydrogen and evolved away from the main sequence. This red giant has nearly double the Sun's mass and has expanded to an estimated radius of over ten times the radius of the Sun, giving it a luminosity of about 54 times the Sun. It is about a billion years old. Unusually for a class G giant, it is cyanogen- deficient and carbon-deficient.

The western portion of Hydra, with Alphard the brightest star near the centre Alphard has three times the mass of the Sun. Its estimated age is 420 million years and it has evolved away from the main sequence to become a giant star with a spectral classification of K3 and luminosity class between II and III. The angular diameter has been measured using long-baseline interferometry, yielding a value of milliarcseconds, only beaten in it by Betelgeuse and R Doradus. It has expanded to 50 times the radius of the Sun.

42 Librae is a single star located around 370 light years distant from the Sun in the southern zodiac constellation of Libra. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.97. This object is drifting closer to the Earth with a heliocentric radial velocity of −22 km/s. This is an aging giant star with a stellar classification of K3-III CN2, where the suffix notation indicates this is a strong CN star with a high overabundance of cyanogen in its spectrum.

37 Librae is a single star in the southern zodiac constellation of Libra. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.61. The star is located 94 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +49 km/s. This is an evolving subgiant star with a stellar classification of K1 III–IV, where the luminosity class indicates the spectrum displays blended traits of a subgiant and a giant star.

Gacrux , Gamma Crucis (Latinised from γ Crucis, abbreviated Gamma Cru, γ Cru), is the nearest class M giant star to the Sun. With an apparent visual magnitude of +1.63, it is the third-brightest star (hence its name) in the southern constellation of Crux (the Southern Cross) and is listed 26th of the brightest stars in the night sky. A line from the two "Pointers", Alpha Centauri through Beta Centauri, leads to within 1° north of this star. Distance has been determined using parallax measurements made during the Hipparcos mission, yielding from the Sun.

As of 2013, the pair had an angular separation of 71.20 arc seconds along a position angle of 249°. The primary, component A, is an evolved G-type giant star with a visual magnitude of 3.50 and a stellar classification of G7 III. This is a red clump star, indicating that it is generating energy through the thermonuclear fusion of helium in its core region. Its measured angular diameter is , which, at the estimated distance of Zeta Lupi, yields a physical size of about 10 times the radius of the Sun.

A wide-set red dwarf star is also a part of the system; this star is an Algol-type eclipsing binary star with a period of 19.5 hours; its minimum magnitude is 9.8 and its maximum magnitude is 9.3. β Gem (Pollux) is an orange-hued giant star of magnitude 1.14, 34 light-years from Earth. Pollux has an extrasolar planet revolving around it, as do two other stars in Gemini, HD 50554, and HD 59686. γ Gem (Alhena) is a blue-white hued star of magnitude 1.9, 105 light- years from earth.

The system has a relatively high proper motion, traversing the celestial sphere at the rate of per year along a position angle of 14.51°. The visible component is an evolved K-type giant star, based upon a stellar classification of K2 III assigned by Gray et al. (2006). In contrast, Keenan and McNeil (1989) gave it a somewhat less evolved classification of K2 III–IV. It is about eight billion years old with 12% more mass than the Sun, and has expanded to 4.8 times the Sun's radius.

1 Cancri is a single star in the zodiac constellation of Cancer, positioned near the border with Gemini at a distance of around 470 light years from the Sun. It is barely visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.97. The object is moving further from the Earth with a heliocentric radial velocity of +14 km/s. This is an evolved giant star with a stellar classification of K3− III, having exhausted the hydrogen at its core and expanded.

46 Cancri is a star in the zodiac constellation of Cancer, located around 680 light years away from the Sun. It is a dim, yellow-hued star, near the lower limits of visibility to the naked eye with an apparent visual magnitude of 6.12. The star is moving closer to the Earth with a heliocentric radial velocity of –13.1 km/s. It has a stellar classification of G5 III, matching an aging giant star that has consumed the hydrogen at its core and evolved away from the main sequence.

HD 139357 b is a very massive extrasolar planet or brown dwarf located approximately 390 light years away, orbiting the 6th magnitude K-type giant star HD 139357 in the constellation of Draco. The detection occurred on March 20, 2009, which was the first day of spring. The actual mass and radius of this body remain known, but it has a minimum mass of nearly 10 times that of Jupiter and a radius of probably no more than 1.2 times Jupiter's. Most likely this is a brown dwarf rather than a planet.

This is an aging giant star with a stellar classification of , where the suffix notation indicates the spectrum shows a mild overabundance of the cyano radical. It is a red clump giant, indicating it is on the horizontal branch and is generating energy through helium fusion at its core. The star has 1.2 times the mass of the Sun and, at the age of 4.6 billion years, has expanded to 11 times the Sun's radius. It is radiating 63 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,581 K.

The Necklace Nebula (PN G054.2-03.4) is a 19-trillion-kilometre-wide ( light- year-wide) planetary nebula located about 15,000 light-years away in the northern constellation Sagitta. It was discovered in 2005 from the Isaac Newton Telescope Photometric H-alpha Survey (IPHAS), a ground-based H-alpha planetary nebula study of the North Galactic Plane. The Necklace Nebula is the exploded aftermath of a giant star that came too close to its Sun-like binary companion. The two stars that produced the Necklace Nebula are in a relatively small orbit about each other.

Vindemiatrix is a giant star with a stellar classification of G8 III. With 2.6 times the mass of the Sun, it has reached a stage in its evolution where the hydrogen fuel in its core is exhausted. As a result, it has expanded to over ten times the Sun's girth and is now radiating around 77 times as much luminosity as the Sun. This energy is being emitted from its outer atmosphere at an effective temperature of 5,086 K, which gives it the yellow-hued glow of a G-type star.

79 Cancri is a star in the constellation Cancer, located 400 light years from the Sun. It is just visible to the naked eye as a dim, yellow-hued star with an apparent visual magnitude of 6.04. This object is gradually moving slower to the Earth with a heliocentric radial velocity of −3.2 km/s. This is an aging giant star with a stellar classification of G5 III, which indicates that, at the age of 770 million years, it has exhausted the hydrogen at its core and evolved away from the main sequence.

The visible component is an evolved giant star with a stellar classification of , where the suffix notation indicates a pronounced underabundance of iron in the spectrum. The measured angular diameter of this star, after correction for limb darkening, is . At its estimated distance, this yields a physical size of about 36 times the radius of the Sun. It is radiating 603 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,210 K. The companion is most likely an A-type main-sequence star with a class of A8–9 V.

Epsilon Canis Minoris (ε Canis Minoris) is a suspected binary star system in the equatorial constellation of Canis Minor. It is a fifth magnitude star, which means it is bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of just 3.13 mas as seen from Earth, this star is located roughly 770 light years from the Sun, give or take a 40 light year margin of error. This is an evolved G-type bright giant star with a stellar classification of G6.5 IIb.

This is an evolved giant star with a stellar classification of K1 III. It has a mild barium anomaly, which may indicate this is a binary star system with a white dwarf companion. The interferometry-measured angular diameter of the visible component is about , which, at its estimated distance, equates to a physical radius of about 44 times the radius of the Sun. This star has four times the mass of the Sun and is radiating 761 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,370 K.

The binary nature of this system was determined based on changes in the proper motion of the visible component. Buscombe (1962) gave the white-hued primary a stellar classification of A0 V, indicating it is an A-type main-sequence star. However, Houk and Smith-Moore (1978) list it with a class of A0 III, which would match a more evolved giant star, also of the A-type. It is 339 million years old with a high rate of spin, having a projected rotational velocity of 145 km/s.

Theta Doradus (Theta Dor, θ Doradus, θ Dor) is a solitary star in the southern constellation of Dorado. Based upon an annual parallax shift of 6.64 mas as seen from Earth, it is located around 490 light years from the Sun. With an apparent visual magnitude of +4.82, the star is bright enough to be faintly visible to the naked eye. This is an evolved orange-hued K-type giant star with a stellar classification of , where the suffix indicates it is a chemically peculiar star with a strong CN band.

The planets Janus Prime and Menda are diametrically opposed in orbit around a vast Red Giant star. But while Menda is rich and fertile in the light of the sun, Janus Prime endures everlasting night, its moon causing a permanent solar eclipse. When the Doctor and Sam arrive on Janus Prime, they find themselves in the middle of a war between rival humans colonising the area. The planet is littered with ancient ruins, and the Mendans are using a mysterious hyperspatial link left behind by the planet's former inhabitants.