183 Sentences With "chasma" | Random Sentence Generator

A deep canyon informally named Argo Chasma is seen grazing the limb.

NASA/JHUAPL/SwRI The photo above shows the Serenity Chasma, part of a belt that encircles Charon's equator.

Image: Coprates Chasma, 2014 / NASA/JPL/University of ArizonaResearchers just uncovered an incredible fact about liquid water on Mars.

Measurements of the Serenity Chasma hinted to scientists that Charon once had at least partially liquid water, which then refroze.

Some of the names, such as the Argo Chasma (a canyon) and Kubrick Mons (a mountain), were already in use by astronomers, but the IAU's ruling now makes them official.

The sediments that make up the layers in Candor Chasma, one of the red planet's largest canyons, may have been transported there by water and later eroded away by wind.

Other IAU-approved names include: Argo Chasma is named for the ship sailed by Jason and the Argonauts, in the epic Latin poem Argonautica, during their quest for the Golden Fleece.

Here's the complete listing of the new names:Argo Chasma is named for the ship sailed by Jason and the Argonauts, in the epic Latin poem Argonautica, during their quest for the Golden Fleece.

Mandjet Chasma is named for one of the boats in Egyptian mythology that carried the sun god Ra (Re) across the sky each day — making it one of the earliest mythological examples of a vessel of space travel.

Caleuche Chasma is named for the mythological ghost ship that travels the seas around the small island of Chiloé, off the coast of Chile; according to legend, the Caleuche explores the coastline collecting the dead, who then live aboard it forever.

Multiple views of Serenity Chasma allowed NASA to create topographical maps of this expanse, and its features are consistent with this proposed geological process; measurements suggest that Charon's water ice layer was at least partially liquid in its early history, and has since refrozen.

Dorothy Crater recognizes the protagonist in the series of children's novels, by L. Frank Baum, that follows Dorothy Gale's travels to and adventures in the magical world of Oz. Mandjet Chasma is named for one of the boats in Egyptian mythology that carried the sun god Ra (Re) across the sky each day — making it one of the earliest mythological examples of a vessel of space travel.

In the middle of the system are very wide valleys of Ophir Chasma (north), Candor Chasma, and Melas Chasma (south). Going farther to the east, one comes to Coprates Chasma. At the end of Coprates Chasma, the valley gets wider to form Capri Chasma in the north and Eos Chasma in the south. The walls of the canyons often contain many layers.

Valles Marineris was discovered by and named for the Mariner 9 mission. Moving east from Noctis Labyrinthus, the canyon splits into two troughs, Tithonium and Ius Chasma in the south. In the middle of the system are very wide valleys of Ophir Chasma (north), Candor Chasma, and Melas Chasma (south) and farther to the east is Coprates Chasma. At the end of Coprates Chasma, the valley gets wider to form Capri Chasma in the north and Eos Chasma in the south.

Valles Marineris was discovered by and named for the Mariner 9 mission. Moving east from Noctis Labyrinthus, the canyon splits into two troughs, Tithonium and Ius Chasma in the south. In the middle of the system are very wide valleys of Ophir Chasma (north), Candor Chasma, and Melas Chasma (south). Going farther to the east, one comes to Coprates Chasma.

The word chasma has been designated by the International Astronomical Union to refer to an elongate, steep-sided depression. Valles Marineris was discovered by and named for the Mariner 9 mission. Moving east from Noctis Labyrinthus, the canyon splits into two troughs, Tithonium and Ius Chasma in the south. In the middle of the system are very wide valleys of Ophir Chasma (north), Candor Chasma, and Melas Chasma (south).

Going farther to the east, one comes to Coprates Chasma. At the end of Coprates Chasma, the valley gets wider to form Capri Chasma in the north and Eos Chasma in the south. The walls of the canyons often contain many layers. The floors of some of the canyons contain large deposits of layered materials.

Mandjet Chasma is a chasma on Pluto's moon, Charon. Mandjet Chasma is long, and about deep, its typical width is . The chasma is part of a global tectonic belt; a series of canyons, scarps, and troughs that traverse the face of Charon along the northern edge of Vulcan Planum. The feature was discovered using stereoscopic processing of New Horizons images.

Starting at the west with Noctis Labyrinthus in the Phoenicis Lacus quadrangle, the canyon system ends in the Margaritifer Sinus quadrangle with Capri Chasma and Eos Chasma (in the south). The word chasma has been designated by the International Astronomical Union to refer to an elongate, steep-sided depression. Valles Marineris was discovered by and named for the Mariner 9 mission. Moving east from Noctis Labyrinthus, the canyon splits into two parallel troughs, Tithonium Chasma to the North and Ius Chasma to the south.

There are two distinct subregions in Planum Australe - Australe Lingula and Promethei Lingula. It is dissected by canyons Promethei Chasma, Ultimum Chasma, Chasma Australe and Australe Sulci. It is theorised that these canyons were created by katabatic wind. The largest crater in Planum Australe is McMurdo Crater.

Hebes Chasma by Mars Express Hebes Chasma is an isolated chasma just north of the Valles Marineris canyon system of Mars. It is centered at 1 degree southern latitude and 76 degrees western longitude, just between the Martian equator and the Valles Marineris system, just east of the Tharsis region.

MOLA altimetry data. Image shows Coprates Chasma, with Melas Chasma at the top, Candor Chasma at top right, and part of Capri Chasma at the bottom Topographic map of Valles Marineris with its associated outflow channels and their surroundings, based on MOLA altimetry data There have been many different theories about the formation of Valles Marineris that have changed over the years.Cabrol, N. and E. Grin (eds.). 2010. Lakes on Mars. Elsevier.

Juventae Chasma is an enormous box canyon (250 km × 100 km) on Mars which opens to the north and forms the outflow channel Maja Valles.PIA03818: Floor of Juventae Chasma Juventae Chasma is located north of Valles Marineris in the Coprates quadrangle and cuts more than 5 km into the plains of Lunae Planum.

At the end of Coprates Chasma, the valley gets wider to form Capri Chasma in the north and Eos Chasma in the south. The walls of the canyons often contain many layers. The floors of some of the canyons contain large deposits of layered materials. Some researchers believe that the layers were formed when water once filled the canyons.

Tethys and Ithaca Chasma Ithaca Chasma is a valley (graben) of Saturn's moon Tethys, named after the island of Ithaca, in Greece. It is up to 100 km wide, 3 to 5 km deep and 2,000 km long, running approximately three-quarters of the way around Tethys' circumference, making it one of the longer valleys in the Solar System. Ithaca Chasma is approximately concentric with Odysseus crater. Ithaca Chasma may have originated when the global salt water ocean inside Tethys froze.

Parts of the floors of Candor Chasma and Juventae Chasma contain interior layered deposits. These layers may have formed when the whole area was a giant lake. However, many other ideas have been advanced to explain them. High-resolution structural and geologic mapping in west Candor Chasma, presented in March 2015, showed that the deposits on the floor of the Candor chasma are basin filling sediments that were deposited in a wet playa like setting; hence water was involved in their formation.

Serenity Chasma is long, and about deep, and its typical width is . The northern wall continues for an additional as a scarp after exiting the chasma. The chasma is part of a global techtonic belt; a series of canyons, scarps, and troughs that traverse the face of Charon. This series of faults is the longest known in the solar system.

The 2,000 km long Ithaca Chasma on Tethys in the Saturn system is a prominent example. Charon's Nostromo Chasma is the first confirmed in the Pluto system, however large chasms up to 950 km wide observed on Charon have also been tentatively interpreted by some as giant rifts, and similar formations have also been noted on Pluto. A recent study suggests a complex system of ancient lunar rift valleys, including Vallis Rheita and Vallis Alpes. The Uranus system also has prominent examples, with large 'chasma' believed to be giant rift valley systems, most notably the 1492 km long Messina Chasma on Titania, 622 km Kachina Chasmata on Ariel, Verona Rupes on Miranda, and Mommur Chasma on Oberon.

Tithonium Chasma is a major part of the largest canyon system in the solar system; this great canyon would go almost all the way across the United States. The name for the whole system of canyons is Valles Marineris. Starting at the west with Noctis Labyrinthus in the Phoenicis Lacus quadrangle, the canyon system ends in the Margaritifer Sinus quadrangle with Capri Chasma and Eos Chasma (in the south). The word Chasma has been designated by the International Astronomical Union to refer to an elongate, steep-sided depression.

Parts of the floors of Candor Chasma and Juventae Chasma contain layered deposits that have been termed interior layered deposits (ILD's) and Equatorial Layered Deposits (ELD's). These layers may have formed when the whole area was a giant lake. However, many other ideas have been advanced to explain them. High-resolution structural and geologic mapping in west Candor Chasma, presented in March 2015, showed that the deposits on the floor of the Candor chasma are basin filling sediments that were deposited in a wet playa like setting; hence water was involved in their formation.

Ganis Chasma consists of a group of rift zones located in the Ganiki Planitia Quadrangle on Venus. A chasma is defined as a long, narrow, steep sided depression on a planet. These depressions, or canyons, formed as a result of extensional tectonics due to volcanism. Ganis Chasma is associated with volcanism of Sapas Mons, a coronae feature located in the Alta Regio region of Venus.

The second major feature seen on Tethys is a huge valley called Ithaca Chasma, about 100 km wide and 3 km deep. It is more than 2000 km in length, approximately 3/4 of the way around Tethys' circumference. Ithaca Chasma occupies about 10% of the surface of Tethys. It is approximately concentric with Odysseus—a pole of Ithaca Chasma lies only approximately 20° from the crater.

Reitia Chasma, a geological feature on the planet Venus, is named after Reitia.

Ithaca Chasma is a giant trough system about 3 km deep and approximately confined to a great circle running through the poles of Tethys. It is approximately concentric with Odysseus impact crater—a pole of Ithaca Chasma lies only approximately 20° from it. The chasma has a rather complex structure consisting of two narrow branches towards the south. Its exterior walls are made of multiple sub-parallel scarps and terraces.

The large troughs present in each pole, Chasma Boreale and Chasma Australe, have both been argued to have been formed by meltwater release from beneath polar ice, as in a terrestrial jökulhlaup.Clifford, S.M. (1987). "Basal polar melting on Mars". J. Geophys. Res.

Some are free-standing mesas and mounds. Interior layered deposits are up to 9 km thick. Parts of the floors of Candor Chasma and Juventae Chasma contain interior layered deposits. These layers may have formed when the whole area was a giant lake.

This is interpreted to be stream-carved plateau deposits and material transported and deposited by flowing fluid. Gangis Chasma is an offshoot chasma of Eos in a general east–west trend. The floor of Gangis is mainly composed of alluvial deposits from the canyon walls.

There have also been Hindu temples and Gurudwaras at Chasma Sahib, Sultanpur, Jalalabad, Ghazni, Helmand (Lashkerga).

This would have caused the surface to crack in order to accommodate the resulting increase in volume. Another hypothesis is that Ithaca Chasma is the outermost ring of the Odysseus impact basin. The chasma is from 4 to 0.4 billion years old, and slightly older than Odysseus.

At some places the chasma has a rim standing as high as 0.5 km about the surrounding cratered plains. Its width varies from only a few kilometers at some places to more than 100 km. The age of Ithaca Chasma is estimated to be either 4.0 or 0.4–3.3 billion years depending on chosen impact chronology. The crater counts indicate that the chasma is slightly older than Odysseus crater but much younger than the cratered plains.

Perspective view of Dali Chasma and Latona Corona on Venus. The Dali and Diana Chasma system consist of deep troughs that extend for and are very distinct features on Venus. Those chasma connect the Ovda Regio and Thetis Regio highlands with the large volcanoes at Atla Regio and thus are considered to be the "Scorpion Tail" of Aphrodite Terra. The broad, curving scarp resembles some of Earth's subduction zones where crustal plates are pushed over each other.

Seasonal flows on Coprates Chasma in Valles Marineris. Deposits from landslides moving in opposite directions meet on the canyon floor near the junction of Melas and Coprates chasmata. Further to the east, the canyon system runs into Coprates Chasma, which is very similar to Ius and Tithonium chasmata. Coprates differs from Ius in the eastern end which contains alluvial deposits and eolian material and like Ius, has layered deposits, although the deposits in the Coprates Chasma are much more well defined.

Ganis Chasma has undergone additional deformation due to pit crater chains that induced fracturing along the rift zone.

Channels near the rim of Ius Chasma, as seen by HiRISE. The pattern and high density of these channels support precipitation as the source of the water. Location is Coprates quadrangle. Research, in the January 2010 issue of Icarus, described strong evidence for sustained precipitation in the area around Ius Chasma.

Eos Chaos is a part of the largest canyon system in the solar system; this great canyon would go almost all the way across the United States. The name for the whole system of canyons is Valles Marineris. Starting at the west with Noctis Labyrinthus in the Phoenicis Lacus quadrangle, the canyon system ends in the Margaritifer Sinus quadrangle with Capri Chasma and Eos Chasma (in the south). The word Chasma has been designated by the International Astronomical Union to refer to an elongate, steep-sided depression.

Capri Mensa is a mesa in the largest canyon system in the solar system; this great canyon would go almost all the way across the United States. The name for the whole system of canyons is Valles Marineris. Starting at the west with Noctis Labyrinthus in the Phoenicis Lacus quadrangle, the canyon system ends in the Margaritifer Sinus quadrangle with Capri Chasma and Eos Chasma (in the south). The word Chasma has been designated by the International Astronomical Union to refer to an elongate, steep-sided depression.

Candor Chasma is one of the largest canyons in the Valles Marineris canyon system on Mars. The feature is geographically divided into two halves: East and West Candor Chasmas, respectively. It is unclear how the canyon originally formed; one theory is that it was expanded and deepened by tectonic processes similar to a graben, while another suggests that it was formed by subsurface water erosion similar to a karst.ESA - Mars Express - Walls of Candor Chasma MRO discovered sulfates, hydrated sulfates, and iron oxides in Candor Chasma.

Serenity Chasma formed as the result of a subsurface ocean on Charon, which expanded as it froze. This expansion pushed the Oz Terra region higher and produced the fault belt across Charon's equatorial region. Landslides have been observed within Serenity Chasma. This is the only known occurrence of landslides in the Kuiper Belt.

Red Cliffs of Mars, at the Chasma Boreale. 2008 photo by HiRISE. Chasma Boreale is a large canyon in Mars's north polar ice cap in the Mare Boreum quadrangle of Mars at 83° north latitude and 47.1° west longitude. It is about long and was named after a classical albedo feature name.

Map of Coprates quadrangle showing details of Valles Marineris, the largest canyon system in the solar system. Some of the canyons may have once been filled with water. Ius Chasma is a major part of Valles Marineris, the largest canyon system in the solar system; this great canyon would go almost all the way across the United States. Starting at the west with Noctis Labyrinthus in the Phoenicis Lacus quadrangle, the canyon system ends in the Margaritifer Sinus quadrangle with Capri Chasma and Eos Chasma (in the south).

There is another theory about the formation of Ithaca Chasma: when the impact that caused the great crater Odysseus occurred, the shock wave traveled through Tethys and fractured the icy, brittle surface. In this case Ithaca Chasma would be the outermost ring graben of Odysseus. However, age determination based on crater counts in high-resolution Cassini images showed that Ithaca Chasma is older than Odysseus making the impact hypothesis unlikely. The smooth plains on the trailing hemisphere are approximately antipodal to Odysseus, although they extend about 60° to the northeast from the exact antipode.

The chasma was first imaged by Voyager 2 spacecraft in January 1986. The Gazetteer of Planetary Nomenclature states that Mommur Chasma is named after the forest home of the fairy king Oberon in A Midsummer Night's Dream. In fact, Oberon's home is not named in Shakespeare's play; it appears instead in the French epic Huon of Bordeaux.

Rim of Ganges chasma, closeup showing stratigraphy and small landslides. Further to the east lie Eos and Ganges chasmata. Eos Chasma's western floor is mainly composed of an etched massive material composed of either volcanic or eolian deposits later eroded by the Martian wind. The eastern end of the Eos chasma has a large area of streamlined bars and longitudinal striations.

It is up to wide and features scarps up to high. By comparison, the Grand Canyon is approximately deep in some places and long but only up to wide. Chasma Boreale cuts through polar deposits and ice, such as those present at Greenland. Planum Boreum interfaces with Vastitas Borealis west of Chasma Boreale at an irregular scarp named Rupes Tenuis.

However, age determination based on crater counts in high resolution Cassini images showed that Ithaca Chasma is older than Odysseus, making the impact hypothesis unlikely.

Ganis Chasma was formed due to extension associated with volcanism in Alta Regio. It formed in the shape of an arc around the Sapas Mons, a corona feature associated with Alta Regio. There are two types of rift structures on Venus, rifts (or chasmata), and fracture belts. Ganis Chasma is younger than other chasmata on Venus, as evidenced by the lack of associated wrinkle ridges.

The immense trench called Ithaca Chasma, which approximately follows a great circle with a pole near Odysseus' center, had been hypothesized to have formed as a result of the Odysseus impact. However, a study based on high resolution Cassini images indicated that this is unlikely—the crater counts inside Odysseus appear to be lower than in Ithaca Chasma, indicating that the latter is older than the former.

THEMIS infrared images, with part of Candor Chasma at bottom Ophir Chasma is a canyon in the Coprates quadrangle of Mars at 4° south latitude and 72.5° west longitude. It is about 317 km long and was named after Ophir, a land mentioned in the Bible. In the Bible it was the land which King Solomon sent an expedition that returned with gold.Blunck, J. 1982.

In planetary nomenclature, a chasma (plural: chasmata ) is a deep, elongated, steep-sided depression. As of 2020, the IAU has named 122 such features in the Solar System, on Venus (63), Mars (25), Saturn's satellites Mimas (6), Tethys (2), Dione (8) and Rhea (5), Uranus's satellites Ariel (7), Titania (2) and Oberon (1) and Pluto's satellite Charon (3). An example is Eos Chasma on Mars.

The Artemis Chasma is the nearly circular fracture in Venus's surface which almost encloses Artemis Corona. The chasma and its associating corona can be found on the Aphrodite Terra continent, at Latitude 35° South, Longitude 135° East. It is named after the Artemis, the Greek virgin goddess of the hunt and the Moon, the hills, the forest, birth, virginity, and fertility, who carries a bow and arrow.

Ganges Mensa is a mesa that sits in a deep upstream basin of the peripheral Ganges Chasma arm of the Valles Marineris valley network. It stretches for nearly from east to west and to the north and south between the walls of Ganges Chasma, bounded to the north by a sharp escarpment and gradually tapering towards the valley floor on the south. At its peak, the mesa rises up to from the Ganges Chasma floor, and its profile has an average elevation of from the valley floor. Ganges Mensa and Hebes Mensa are the only mesas of Valles Marineris that extend to the height of the surrounding plateau terrain.

The bottom of the Coprates Chasma contain a large field of small pitted cones which have been interpreted as Martian equivalents of terrestrial igneous or mud volcanoes.

Asteria Regio is a region on the planet Venus. It is bordered on the southeast by Phoebe Regio. It is located in the Hecate Chasma (v28) quadrangle.

Ius Chasma image mosaic from 2001 Mars Odyssey, showing side canyons created by sapping. On the northern (upper) rim, right of center, a side canyon turns 90 degrees where it encounters a graben. Further to the east from Oudemans, Ius and Tithonium chasmata are located parallel to each other, Ius to the south and Tithonium to the north. Ius is the wider of the two, leading to Melas Chasma.

False color HiRISE image of a side of the Chasma Boreale, a canyon in the polar ice cap. Light browns are layers of surface dust greys and blues are layers of water and carbon dioxide ice. Regular geometric cracking is indicative of higher concentrations of water ice. The main feature of the Planum Boreum is a large fissure or canyon in the polar ice cap called Chasma Boreale.

The Thaumasia Plateau lies at the heart of the Tharsis Rise, and is framed to the northwest by the Noctis Labyrinthus fracture zone and the Valles Marineris chasmata (particularly, Ius Chasma, Melas Chasma, and Coprates Chasma, from northwest to northeast). Older Noachian basement crust, likely predating the formation of Tharsis, bound the Thaumasia Plateau to the west (Claritas Rise and the Claritas Fossae), the south (Thaumasia highlands), and the east (Coprates Rise and the Nectaris Fossae). The plateau stretches over 2900 km across the surface of Mars and sits at around a 4 km relief relative to the southern highland terrains immediately surrounding the Tharsis Rise. There are two general provinces composing the Thaumasia Plateau.

The youngest unit lies within Odysseus crater with an estimated age from 3.76 to 1.06 billion years, depending on the absolute chronology used. Ithaca Chasma is older than Odysseus.

This region has been interpreted as a chaos terrain or a mantled, eroded remnant of volcanic edifices. The moat-like region to the north of the mesa province is dominated by landslide terrains from collapses in the Ganges Chasma canyon wall. Some of this area has since been mantled by sand dune cover. Researchers have also reported evidence for sulfate signatures manifesting in light-toned mounds that can be observed across the Ganges Chasma floor.

Voyager 2 image of Oberon showing Mommur Chasma near the limb at upper right. Mommur Chasma is the largest 'canyon' on the known part of the surface of Uranus' moon Oberon. This feature probably formed during crustal extension at the early stages of moon's evolution, when the interior of Oberon expanded and its ice crust cracked as a result. The canyon is an example of graben (rift valley) or scarp produced by normal fault(s).

It extends from latitude 77.12°N to 82.8°N and from longitude 302.92°E to 316.02°E (43.98°W – 57.08°W). Its centre is at latitude 79.96°N, longitude 49.49°W, and has a diameter of . Hyperboreae Undae is southwest of the Boreum Cavus depression, an arc-like depression at the northeastern boundary of Chasma Boreale. From there, Hyperboreae Undae continues in a southwestern direction through Chasma Boreale, and into the lowlands of Vastitas Borealis.

His famous songs include "Aaja Ni Aaja", " Kaala Chasma" and "Rangli Kothi". "Kala Chashma" song was remixed for a Bollywood movie Baar Baar Dekho (2016), which was a huge success.

The more dust, the darker the surface. The darker the surface, the more melting. Dark surfaces absorb more light energy. One large valley, Chasma Boreale runs halfway across the cap.

Okubo, C. 2015. HIGH-RESOLUTION STRUCTURAL AND GEOLOGIC MAPPING IN CANDOR CHASMA. 46th Lunar and Planetary Science Conference. 1210.pdf Some places on Mars contain hydrated sulfate deposits, including ILD's.

Ophir Chasma THEMIS mosaic The next portion of Valles Marineris to the east are three chasmata, that from south to north are Melas, Candor and Ophir chasmata. Melas is east of Ius, Candor is east of Tithonium and Ophir appears as an oval that runs into Candor. All three chasmata are connected. The floor of Melas Chasma is about 70% younger massive material that is thought to be volcanic ash whipped up by the wind into eolian features.

In the modern era, eponyms and literary allusions to Dali indicate the persistence of her narrative in the cultural memory. The Dali Chasma and the Tkashi-mapa Chasma on Venus are named for Dali and her Mingrelian equivalent Tkashi-Mapa. Capra dalii, a fossil species of goat discovered in Georgia, is named for Dali. Fragments of Capra dalii fossils were first located at the Dmanisi archaeological site in 2006, and are believed to be related to the west Caucasian tur, Capra caucasica.

Tithonium Chasma is a large canyon in the Coprates quadrangle of Mars at 4.6° south latitude and 84.7° west longitude. It is about 810 km long and was named after a classical albedo feature.

Some of the canyons may have once been filled with water. Candor Chasma is in the middle. One of the pictures below shows branched channels. Many places on Mars show channels of different sizes.

Ius Chasma is a large canyon in the Coprates quadrangle of Mars at 7° south latitude and 85.8° west longitude. It is about 938 km long and was named after a classical albedo feature name.

The rifts that make up Ganis Chasma formed in the shape of an arc along the edge of Sapas Mons, orientated in a north–south direction. Little is known about ongoing volcanic activity on Venus. So far, no volcanic activity has been determined to have occurred in the last two million years. In 2008 and 2009 images taken by the Venus Monitoring Camera on the European Space Agency's (ESA) Venus Express (VEx) in eight observational sessions detected four bright transient spots along the edges of Ganis Chasma.

The Devana Chasma formed along the Beta Regio and Phoebe Regio volcanic rises,Senske, D.A., J.W. Head, et al. "GEOLOGY AND STRUCTURE OF BETA REGIO, VENUS' RESULTS FROM ARECIBO RADAR IMAGING." GEOPHYSICAL RESEARCH LETTERS. 18.6 (1991): 1159–1162. .

Gallifrey is a dark surface feature on Pluto's moon Charon. It is named after the fictional planet Gallifrey in the television series Doctor Who. As a further homage to Doctor Who, Gallifrey Macula is bisected by Tardis Chasma.

Nostromo Chasma is the unofficial name for a rift valley on Pluto's moon Charon. It was named after the fictional spacecraft in the science- fiction/horror film Alien, which in turn was named after the novel by Joseph Conrad.

Critics of this hypothesis for Ganges Mensa note that there are no barriers in the chasmata that appear to confine a putative paleolake downstream towards the outflow channels that they usually source (such as how Ganges Chasma opens into the uplands of Chryse Planitia), and how there are no observed morphologies on Ganges Mensa or on any of the other mesas of Valles Marineris that could conceivably correspond to paleoshoreline benches. More generally, Hebes Mensa also extends to a higher elevation than the rim of Hebes Chasma, which has implications on the broader formational mechanism of the valley mesas that are unlikely to be explained by a lacustrine mechanism. However, it is entirely possible that resurfacing could have eradicated any sign of such paleoshorelines, and that the geometry of Ganges Chasma might have been different enough in the past to have supported the presence of a deep paleolake.

In 2014, this was interpreted by Eugene Shalygin and his colleagues as active hotspot volcanism. The team suggests that transient bright spots observed in several consequent images of Ganis Chasma is the first direct evidence of current volcanic activity on Venus.

Active volcanism on Venus in the Ganiki Chasma rift zone. E. V. Shalygin, W. J. Markiewicz, A. T. Basilevsky, etal. . 23 May 2015.Shalygin, E. V., Basilevsky, A. T., Markiewicz, W. J., Titov, D. V., Kreslavsky, M. A., & Roatsch, T. (2012).

The resonance would have led to orbital eccentricity and tidal heating that may have warmed Tethys' interior enough to form the ocean. Subsequent freezing of the internal ocean after the moons escaped from the resonance may have generated the extensional stresses that created Ithaca Chasma. An alternative hypothesis is that it was formed at the same time as the large crater Odysseus which lies near a pole of the Ithaca Chasma. When the impact that created Odysseus occurred, the shockwave may have traveled through Tethys and produced a circumcircular fracture analogous to outer ring graben of multiring impact basins.

However, many other ideas have been advanced to explain them. High-resolution structural and geologic mapping in west Candor Chasma, presented in March 2015, showed that the deposits on the floor of the Candor chasma are basin filling sediments that were deposited in a wet playa like setting; hence water was involved in their formation. One problem with the idea of large lakes in Valles Marineris is that there are no evident sources for the huge amount of water that would be required. Although many small channels exist in the region, there are no major channels.

The municipality Larissa has an area of , the municipal unit Larissa has an area of , and the community Larissa has an area of . The Larissa Chasma, a deep gash in the surface of Dione, a natural satellite of Saturn, was named after Larissa.

The slow extension rates in the rift may be driven by the same reason.Kiefer, W. S., and L. C. Swafford. "Topographic Analysis Of Devana Chasma, Venus; Implications For Rift System Segmentation And Propagation." Journal of Structural Geology 28.12 (2006): 2144–2155. GeoRef. Web.

Finer scale valley networks near Candor Chasma, seen by HiRISE (click to zoom). Field of view is roughly 3.5 km across. Surface the valleys are cut into appears to be eroding back. Valley networks are very strongly concentrated in the cratered southern uplands of Mars.

Over the years, it has been suggested that lakes of various sizes existed in the giant Valles Marineris.Lucchitta, B. 2008. HiRISE images of layered deposits in west Candor Chasma, Mars (I): wall rock relations, enigmatic ridges, and possible dikes. 39th Lunar Planet. Sci. Conf.

Hebes Mensa is a large mensa that rises from the floor of Hebes Chasma, one of the chasmata of the Valles Marineris network on Mars. Some researchers have identified this mesa to be an interior layered deposit (ILD), similar to Ganges Mensa, and are named for alternating light-toned and dark-toned layers forming a stair-stepped stratigraphy. The faces of Hebes Mensa are sometimes fluted. Although many researchers have proposed a low-energy lacustrine depositional origin tied to continual groundwater feeding interspersed with occasional subaqueous volcanism, others have contested this hypothesis, noting that Hebes Mensa is so tall that it actually stretches above the canyon walls of Hebes Chasma.

Ganges Mensa (also occasionally termed Gangis Mensa in literature) is a mesa and an interior layered deposit in Ganges Chasma, one of the peripheral valleys of Valles Marineris on Mars. The mesa rises up to from the floor of Ganges Chasma, nearly to the same elevation as the surrounding plateaux of Lunae Planum. Like Hebes Mensa, the mesa is completely separated from the surrounding canyon walls and has sustained significant erosion that has caused it to retreat in areal extent. The mesa is composed of friable, thinly-layered units which decompose into fluted patternations, interpreted by most researchers as erosional aeolian features known as yardangs.

Parts of the floor of Candor Chasma contains layered deposits that have been termed interior layered deposits (ILD's). These layers may have formed when the whole area was a giant lake. Some places on Mars contain hydrated sulfate deposits. Sulfate formation involves the presence of water.

Serenity Chasma is the unofficial name given to a large pull-apart fault on Pluto's moon, Charon. It is part of a series of faults that run along the perimeter of Vulcan Planum. It was discovered by the New Horizons mission, and informally named after the fictitious spaceship, Serenity.

Ursula is a large bright crater near the bottom of this Voyager 2 image. Ursula is a large crater on Uranus's moon Titania. It is about 135 km across, and is cut by Belmont Chasma. It is named after Hero's attendant in William Shakespeare's comedy Much Ado About Nothing.

His diction was unique here is one of his famous ghazal. Yaad karna har ghari us yaar ka Hai wazifa mujh dil-e-bimaar ka. Aarzoo-e-chasma-e-kausar nahin Tishna-lab hun sharbat-e- didaar ka. Aakbat kya howega maalum nahin Dil hua hai mubtla dildaar ka.

A Traveler's Guide to Mars. Workman Publishing. NY NY. The ice cap is surrounded by the vast plains of Planum Boreum and Vastitas Borealis. Close to the pole, there is a large valley, Chasma Boreale, that may have been formed from water melting from the ice cap.Clifford, S. 1987.

From the fountains, water flows along the floor of the pavilion and cascades to a lower terrace over a drop of along a polished black stone chute. A small shrine, known as the Chasma Sahibi, is located in the vicinity of the gardens and has a fresh water spring.

Private institutes include Al-Hudabia Public High School, Minnhaj Public School and Al-Quraish Public School. It has also a veterinary hospital. To facilitate farmer for selling animal a market is held every week on Saturday by government contractor. It is situated at a bank of Chasma road.

These units were deposited in at least two depositional events, interspersed by at least one or possibly two extended periods of erosion, depending on specific interpretations about the presence of angular conformities observed in the stratigraphy. The basal stratigraphic units of Gange Mensa demonstrate spectral signatures of polyhydrated sulfates like kieserite, which are visible up to elevations of uphill on the mesa. These sulfate signatures are not consistently represented elsewhere in the Valles Marineris network but are present within Eos Chasma and Capri Chasma and particularly on Capri Mensa, which lies to the south. Some of these units are scored by what have been interpreted by some researchers to be foreset beds of dark aeolian (wind-formed) materials.

These sulfate signatures are only observed on the upper unit identified by Sowe and her coworkers. In 2011, Mariam Sowe, Gerhard Neukum (Free University of Berlin) and Ralf Jaumann (DLR) published a comparative study of interior layered deposits across Valles Marineris and the region of its debouchment into Chryse Planitia. Ganges Mensa was one of two principal sites (along with Eos Chasma) where these ILDs had been observed and studied in the Valles Marineris network, with the remainder of the studied sites downstream to the northeast. A cross-section of a region including Ganges Mensa and Eos Chasma was prepared in the publication, and the particular formation mechanisms of the ILDs discussed therein.

Coprates Chasma based on THEMIS data Coprates Chasma is a huge canyon in the Coprates quadrangle of Mars, located at 13.4° south latitude and 61.4° west longitude, part of the Valles Marineris canyon system. It is long and was named after a classical albedo feature name. Near 60° W is the deepest point of the Valles Marineris system (as well as its lowest point by elevation) at below the surrounding plateau. Eastward from here there is about a 0.03 degree upward slope before reaching the outflow channels, which means that if you filled the canyon with fluid, it would create a lake with a depth of before the fluid would overflow out onto the northern plains.

Ganis Chasma is a group of rift zones on the surface of the planet Venus. Bright spots detected by the Venus Monitoring Camera on the European Space Agency's Venus Express in the area suggest that there may be active volcanism on Venus. Magellan spacecraft by NASA. Modified after Dinderman (2015).

Location of the Ganiki Planitia Quadrangle Ganis Chasma is located in the Ganiki Planitia Quadrangle. This quadrangle is positioned between two volcanic regions on Venus. To the north lies the Atlanta Planitia lowland which was formed as the result of mantle upwelling and downwelling. To the south lies Alta Regio.

Cattermole, 105 A field of more than 100 pitted cones on the floor of Coprates Chasma has been interpreted as a set of small igneous cinder or tuff cones, with associated lava flows. Crater dating indicates they are of Middle to Late Amazonian age, about 200 to 400 million years old.

This region is a major volcanic rise and was formed as the result of mantle upwelling. The Ganiki Planitia Quadrangle was strongly influenced by mantle flow tectonics derived from these two regions. The area contains many volcanic, tectonic, and impact features. Ganis Chasma is one of the extensional features located in the region.

He also established the food processing and agricultural engineering labs at PAEC. In May 1998, he was awarded Hilal-i-Imtiaz by then-Prime Minister of Pakistan, Nawaz Sharif. He also served as a director of KANUPP Institute of Nuclear Power Engineering before promoting as a director general at the Chasma Reactor.

Area around the Northern Kasei Valles in Mars Express images This huge system is 300 miles wide in some places. In contrast, Earth's Grand Canyon is only 18 miles wide. It is one of the longest continuous outflow channel systems on Mars. The Kasei Valles system begins in Echus Chasma, near Valles Marineris.

Lucchitta and her co-workers noted that there was no evidence that Ganges Chasma was dammed, thus making a lacustrine origin hypothesis unlikely. They first advanced the hypothesis that Ganges Mensa might have been a tuya, a volcanic table mountain formed by eruptions into gigantic pingo-like ice laccoliths or shallow frozen lakes.

From the Dargah, a further hike of 45 minutes to 1 hour, takes you to the graves of " Panch Peer " which are of the disciples of Baba who came with him. Along this stretch, one visits the place of "Chasma". It is believed that from a spot where Baba's horse leg touched, water spouted.

Taarak Mehta Ka Ooltah Chashmah ( Taarak Mehta's Inverted Spectacles) is an Indian Hindi language television sitcom, based on the weekly column called Duniya Ne Undha Chasma by Taarak Mehta in Chitralekha. One of India's longest running television shows, it is produced by Neela Tele Films. It premiered on 28 July 2008 on SAB TV.

There are several graben radiating away from Odysseus, which are 10–20 km wide and hundreds of kilometers long. They are likely to be cracks in the crust created by the impact. The most prominent among them is called Ogygia Chasma. The crater must have originally been deep, with a high mountainous rim and towering central peak.

They are cut by deep troughs across. These troughs are an example of continental rifting, and are evidence of surface tectonism. Beta Regio is cut by a radar-bright north-south trough called Devana Chasma. The northern end has a volcano called Rhea Mons, and the southern end is dominated by a volcano titled Theia Mons.

In some places, it seems that sapping was involved. Here around Ius Chasma, there is evidence for precipitation. If this is true, climate models may need to be modified because some models show that Mars may have been too cold for much liquid water. Many of these channels probably carried water, at least for a time.

A HiRISE image of one of the edges of Ganges Mensa. The dune sea of the floor of Ganges Chasma is visible to the left of the image, with other sand dunes forming dark streaks across Ganges Mensa's cap. Fluted texturations are visible, sloping downwards to the left. Steeper slopes tend to have a lighter texturation in Ganges Mensa.

Hebes Chasma, a large enclosed valley, may have once held water. Hydrated minerals have been found there. It is thought that large-scale underground springs of groundwater at different times burst to the surface to form deposits called Light Toned Deposits (LTD's). Some suggest present or fossilized life forms may be found there because the deposits are relatively young.

Balch is a crater on Venus at latitude 29.9, longitude 282.9 in Devana Chasma, Central Beta Regio. It is 40 km in diameter and named after Emily Balch, though it was originally designated Somerville crater. This crater is one of the few examples of tectonically modified craters seen on Venus. Approximately half the crater was subsumed into a valley.

Cassini view of Mimas's trailing hemisphere, showing craters up to 6 km deep and 1-km-deep chasmata (grooves). The large crater near center is Morgan; Arthur is close to the lower right limb. Pelion Chasma is faintly visible as a horizontal trough left of Arthur and below Morgan. The surface area of Mimas is slightly less than the land area of Spain.

Chasmosaurus ( ) is a genus of ceratopsid dinosaur from the Upper Cretaceous Period of North America. Its name means 'opening lizard', referring to the large openings (fenestrae) in its frill (Greek chasma meaning 'opening' or 'hollow' or 'gulf' and sauros meaning 'lizard'). With a length of and a weight of , Chasmosaurus was a ceratopsian of average size. Like all ceratopsians, it was purely herbivorous.

From the Magellan mission data, 3 types of images have been produced: (1) SAR images, (2) topographic images and (3) meter scale slope image.Kazuo, O. "Recent Trend and Advance of Synthetic Aperture Radar with Selected Topics: Remote Sensing." (2013): 716-807.Graff, Jamie R. MAPPING AND ANALYSIS OF THE TECTONO-MAGMATIC FEATURES ALONG THE HECATE CHASMA RIFT SYSTEM, VENUS. Diss.

Also, the low point in Eos Chasma where water would be expected to overflow is marked by fluvial features. The features look like the flow came together at a small point and carried out significant erosion.Harrison, K., M. Chapman. 2010. Episodic ponding and outburst flooding associated with chaotic terrains in Valles Marineris In Cabrol, N. and E. Grin (eds.). 2010.

3D rendering of a DEM of Tithonium Chasma on Mars A digital elevation model (DEM) is a 3D computer graphics representation of elevation data to represent terrain, commonly of a planet (e.g. Earth), moon, or asteroid. A "global DEM" refers to a discrete global grid. DEMs are used often in geographic information systems, and are the most common basis for digitally produced relief maps.

Map of Coprates quadrangle showing details of Valles Marineris, the largest canyon system in the solar system. Some of the canyons may have once been filled with water. Ophir Chasma is part of the largest canyon system in the solar system; this great canyon would go almost all the way across the United States. The name for the whole system of canyons is Valles Marineris.

The 16th-century mythographer Natale Conti describes Pluto's imperium as "the Spains and all the places bordering the setting sun" (Mythologiae 2.9, edition of 1651, p. 173; cf. Strabo 3.12). In the discourse On Mourning by the Greek author Lucian (2nd century AD), Pluto's "wealth" is the dead he rules over in the abyss (chasma); the name Hades is reserved for the underworld itself.

During the 1173 sol-stay on the Martian surface the crew would carry out a number of expeditions across the polar ice cap. Expeditions to the Chasma Boreale and along the polar spiral valleys were considered in detail. The study also considered the possibility of exploratory mid-winter expeditions across the polar ice cap. These expeditions would be supported by pressurised and unpressurised rovers.

Chasma Australe, a major valley, cuts across the layered deposits in the South Polar cap. On the 90 E side, the deposits rest on a major basin, called Prometheus. Some of the layers in the south pole also show polygonal fracturing in the form of rectangles. It is thought that the fractures were caused by the expansion and contraction of water ice below the surface.

Devana Chasma is a weak extensional rift zone on Venus, with a length of 4000 km, a width of 150–250 km, and a depth reaching 5 km. Most of the faults are facing north–south. The rift is located in Beta Regio, a 3000 km rise created by volcanic activity. Mantle plumes rising from the bottom are the reason behind the formation of the rift zone.

Image of the Coprates Quadrangle (MC-18). The prominent Valles Marineris chasma system intersects the moderately cratered northern part and the faulted highland ridged plains in the southern part. The Coprates quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Coprates quadrangle is also referred to as MC-18 (Mars Chart-18).

Ursula has a central pit with diameter of about 20 km. It is probably one of the youngest large impact craters on Titania. The crater is surrounded by smooth plains, which have the lowest impact crater density of all geological units on the moon, although they are cut by Belmont Chasma. The plains may be impact deposits (ejecta) associated with Ursula or they may be cryovolcanic in origin.

At the southern boundary of Chasma Boreale, a sequence of mounds of Abalos Coles with flat, pitted or cratered tops, show similar morphological characteristics to small Icelandic shield volcanoes of basaltic origin. Adjusted to account for the difference in topology between the two planets, both the terrestrial and Martian volcanoes share similar side slopes and volume to diameter ratios, the latter being defined as the volcanic productivity index.

During the 10th century, pilgrims from Bukhara and other places came to the holy graves situated next to the town fortifications and mosques. Currently, pilgrims continue visiting the holy places. Chashma is a place of pilgrimage of believers and one of the most significant religious centers of Islam in the region. The complex of religious constructions “Chasma” (Tadjik word for spring) includes the spring, a well, mosque “Djuma” and khamom (bathhouse).

However, in 2018, Giovanni Leone of the University of Atacama published a direct rebuttal to this publication, pointing out that Cull-Hearth and Clark had crafted their study around the assumption that the hydrated minerals of Ganges Mensa and Ganges Chasma required aqueous processes to form. Leone cited a variety of publications suggesting alternate explanations for alteration that the original co-authors did not address or otherwise rebut.

Expeditions were planned to numerous locations across the Martian north polar caps, including the Chasma Boreale and the polar layered terrains. The study involved wide-ranging investigations of the scientific priorities for a human presence at the Martian polar ice caps through to detailed architectural and design studies for the station. Studies were undertaken on mobility and communications and psycho-social issues for long-term operation at the Martian polar station.

It has also been suggested that Venusian lightning (discussed below) could originate from volcanic activity (i.e. volcanic lightning). In January 2020, astronomers reported evidence that suggests that Venus is currently volcanically active. In 2008 and 2009, the first direct evidence for ongoing volcanism was observed by Venus Express, in the form of four transient localized infrared hot spots within the rift zone Ganis Chasma, near the shield volcano Maat Mons.

North Polar ice cap, Korolov crater and Chasma Boreale. The Mare Boreum quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Mare Boreum quadrangle is also referred to as MC-1 (Mars Chart-1).Davies, M.E.; Batson, R.M.; Wu, S.S.C. "Geodesy and Cartography" in Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W.; Matthews, M.S., Eds. Mars.

Arsia Chasmata is a steep-sided depression located northeast of Arsia Mons in the Phoenicis Lacus quadrangle on Mars, located at 7.6° S and 119.3° W. It is 97 km long and was named after an albedo name. Arsia Chasmata, as seen by HiRISE. A pit crater chain is visible in the lower right. In planetary geology, a chasma (plural: chasmata) is a deep, elongated, steep-sided depression.

However, the story also portrays the life of the wife who suffered greatly without her husband. Other stories by Bishweshwar Prasad Koirala introduced psychology into literature, for instance through creations such as "Teen Ghumti", "Doshi Chasma" and "Narendra Dai". This regime produced several prominent poets such as, Laxmi Prasad Devkota, Gopal Prasad Rimal, Siddhicharan Shrestha, Bhim Nidhi Tiwari and Balkrishna Sama. Later, several poets come into light during the Panchayat regime.

But at the same time there are also some large basins that are not associated with such positive Bouguer anomaly, for example, Daedalia, northern Tharsis and Elysium, which are believed to be underlain by the northern lowland plain. In addition, certain portions of Coprates, Eos Chasma and Kasei Valles are also found to have positive Bouguer anomalies, though they are topographic depressions. This may suggest that these depressions are underlain by shallow dense intrusion body.

A small amount of an unidentified dark material is present as well. The surface of Tethys is very bright, being the second-brightest of the moons of Saturn after Enceladus, and neutral in color. Tethys is heavily cratered and cut by a number of large faults/graben. The largest impact crater, Odysseus, is about 400 km in diameter, whereas the largest graben, Ithaca Chasma, is about 100 km wide and more than 2000 km long.

Venera 9 landed within a radius of , near Beta Regio, on a steep (20°) slope covered with boulders (suspected to be the slope of the tectonic rift valley, Aikhylu Chasma). The entry sphere weighed and the surface payload was .Interplanetary Spacecraft It was the first spacecraft to return an image from the surface of another planet. Many of the instruments began working immediately after touchdown and the cameras were operational 2 minutes later.

105 Artemis, the Artemis (crater), the Artemis Chasma, the Artemis Corona, and the Artemis lunar program have all been named after the goddess. Artemis is the acronym for "Architectures de bolometres pour des Telescopes a grand champ de vue dans le domaine sub-Millimetrique au Sol", a large bolometer camera in the submillimeter range that was installed in 2010 at the Atacama Pathfinder Experiment (APEX), located in the Atacama Desert in northern Chile.

27 Feb. 2014. Evidences from the images of the Beta Regio shows the history behind the region, the rise of the region is caused by an uplift of the mantle plume, which caused the formation of Theia Mons shield volcano. The Devana Chasma rift system were also constructed by the uplift, and became active due to the Theia Mons volcano. Furthermore, these evidences proposed several aspects concerning the development and history of the rift zone.

Locations of observed transient bright spots on Ganis Chasma, Venus. Modified from Shalygin (2014) Previous studies have been conducted in search of current volcanic activity on Venus. These include observing increases in the amount of sulfur dioxide, a gas emitted by volcanoes, in Venus's upper atmosphere as well as observing possible lava flows emitting heat on Venus's surface. While these studies indicate presence of past volcanic activity, none could prove any volcanism occurring in the past 2 million years.

Extraterrestrial rift valleys are also known to occur on other terrestrial planets and natural satellites. The 4,000 km long Valles Marineris on Mars is believed by planetary geologists to be a large rift system. Some features of Venus, most notably, the 4,000 km Devana Chasma and a part of the western Eistla, and possibly also Alta and Bell Regio have been interpreted by some planetary geologists as rift valleys. Some natural satellites also have prominent rift valleys.

Images of rocks in the canyon walls almost always show layers. Some layers appear tougher than others. In the image below of Ganges Chasma Layers, as seen by HiRISE, one can see that the upper, light-toned deposits are eroding much faster than the lower darker layers. Some cliffs on Mars show a few darker layers standing out and often breaking into large pieces; these are thought to be hard volcanic rock instead of soft ash deposits.

Nasreddin is a crater on Pluto's largest moon, Charon. The crater was first observed by NASA's New Horizons space probe on its flyby of Pluto in 2015. The name was chosen as a reference to Nasreddin, the hero of humorous folktales told throughout the Middle East, southern Europe and parts of Asia. The location of Nasreddin crater is in the northern Pluto-facing hemisphere of Charon, north of Mandjet Chasma in a region informally called Oz Terra.

There are two basic hypothesis as to how Ithaca Chasma formed. One of them is that it formed as Tethys' internal global liquid salt water ocean solidified, causing the moon to expand and cracking its surface to accommodate the extra volume within. Earlier craters made before Tethys solidified were probably all erased by geological activity before then. Tethys' global subsurface ocean may have resulted from a 2:3 orbital resonance between this moon and Dione early in the Solar System's history.

The largest of the northern troughs is named Saturnalia Fossa (≈ 40 km wide, > 370 km long). These troughs are thought to be large-scale graben resulting from the impacts that created Rheasilvia and Veneneia craters, respectively. They are some of the longest chasms in the Solar System, nearly as long as Ithaca Chasma on Tethys. The troughs may be graben that formed after another asteroid collided with Vesta, a process that can happen only in a body that, like Vesta, is differentiated.

Since 1967, France has emerged as the biggest defence contractor of Pakistan, despite its good and relatively close relations with India. Pakistan is one of three original participant states (others being India and Israel) that refused to be signatory of the NPT.See: Nuclear Proliferation Treaty On March 1976, France and Pakistan signed a mutual agreement for the supply of plutonium- based nuclear reprocessing plant at the Chasma. However, this deal came under attack from various countries, particularly the United States, for two reasons.

More unusual origins are also possible. For example, the Geryon Montes of Mars are an erosional remnant of a former plateau within Ius Chasma, part of the Valles Marineris canyon system. During impact events, mountains can appear not only on the border of the resulting crater, but also in its center. Classical central peaks generally are not named, although some peaks within craters are named: for example, Aeolis Mons within Gale crater on Mars or the Scheria Montes within Odysseus crater on Tethys.

Chasma Boreale is a canyon-like feature older than the troughs, and in contrast is aligned parallel to the wind direction. The surface composition of the northern ice cap in middle spring (after a winter's accumulation of seasonal dry ice) has been studied from orbit. The outer edges of the ice cap are contaminated with dust (0.15% by weight) and are mostly water ice. As one moves toward the pole, the surface water ice content decreases and is replaced by dry ice.

Four temporally variable surface hotspots were discovered at the Ganiki Chasma rift zone near volcanoes Ozza Mons and Maat Mons in 2015, suggestive of present volcanic activity.Highly Volcanic Exoplanets, Lava Worlds, and Magma Ocean Worlds: An Emerging Class of Dynamic Exoplanets of Significant Scientific Priority. Wade G. Henning1, Joseph P. Renaud, Prabal Saxena, etal. A white paper submitted in response to the National Academy of Sciences 2018 Exoplanet Science Strategy solicitation, from the NASA Sellers Exoplanet Environments Collaboration (SEEC) of the Goddard Space Flight Center.

Keith Harrison and Mary Chapman described strong evidence for a lake in the eastern part of Valles Marineris, especially in Coprates Chasma. It would have had an average depth of only 842 m—much smaller than the 5–10 km depth of parts of Valles Marineris. Still, its volume of 110,000 cubic miles would be comparable to Earth’s Caspian and Black Seas. The main evidence for such a lake is the presence of benches at the level that models show is where the lake level should be.

In 2012, Gillani attended the 2012 Nuclear Security Summit where he defended the right of Pakistan's access to nuclear technology for peaceful uses on a non-discriminatory basis. His government announced the approval the safeguards agreements of the two commercial civil nuclear power plants, and inaugurated the CHASNUPP-III nuclear power plant in Chasma. In 2012, Gillani gave approval of establishing two civilian nuclear power plant in Karachi to meet the future energy needs of financial and economical development. On 9 April 2012, Gillani chaired the second energy conference held in Lahore.

Tarak Janubhai Mehta was an Indian columnist, humourist, writer and playwright who is best known for the column Duniya Ne Undha Chasma. He translated and adapted several comedies into Gujarati, and was a well-known figure in the Gujarati theatre. His humourous weekly column first appeared in Chitralekha in March 1971 and looked at contemporary issues from a different perspective. He published 80 books; three were based on the columns he wrote in the Gujarati newspaper Divya Bhaskar while the rest were compiled from the stories in Taarak Mehta Ka Ooltah Chashmah.

Ius has a ridge down the center of it by the name of Geryon Montes, composed of the undivided basement rock. The floor of Ius Chasma is mostly composed of pristine landslide material, not much degraded by cratering or erosion. The southern wall of Ius, and to a lesser extent the northern wall, has many short valleys stretching off roughly perpendicular to the line of the chasmas. These valleys have a stubby theater- headed leading edge very much like features seen on the Colorado Plateau near the Grand Canyon that appear from groundwater sapping.

The Elixir has had hundreds of names (one scholar of Chinese history reportedly found over 1,000 names for it), among them Amrit Ras or Amrita, Aab-i-Hayat, Maha Ras, Aab-Haiwan, Dancing Water, Chasma-i-Kausar, Mansarover or the Pool of Nectar, Philosopher's stone, and Soma Ras. The word elixir was not used until the 7th century A.D. and derives from the Arabic name for miracle substances, "al iksir". Some view it as a metaphor for the spirit of God (e.g., Jesus's reference to "the Water of Life" or "the Fountain of Life").

East of Eos and Ganges, Valles Marineris empties out into the Chryse region of the northern plains of Mars at an elevation only above the deepest point of Valles Marineris in Melas Chasma. The outflow regions of the northern plains are similar to the terrain seen at the Mars Pathfinder landing site. A terrestrial counterpart of these outflow channels on Earth would be the scablands of eastern Washington. The eastern Washington scablands are a result of repeated catastrophic flooding due to the build-up of an ice dam at the head of Lake Missoula in the Late Pleistocene.

Tectonic fractures within the Candor Chasma region of Valles Marineris, Mars, retain ridge-like shapes as the surrounding bedrock erodes away. This points to past episodes of fluid alteration along the fractures and reveals clues into past fluid flow and geochemical conditions below the surface. On September 29, 2006 (sol ), MRO took its first high resolution image from its science orbit. This image is said to resolve items as small as 90 cm (3 feet) in diameter. On October 6, NASA released detailed pictures from the MRO of Victoria crater along with the Opportunity rover on the rim above it.

The surface of Tethys mostly consists of hilly cratered terrain dominated by craters more than 40 km in diameter. A smaller portion of the surface is represented by the smooth plains on the trailing hemisphere. There are also a number of tectonic features such as chasmata and troughs. Cassini view of Tethys's Saturn-facing hemisphere, showing the giant rift Ithaca Chasma, crater Telemachus at top, and smooth plains at right The western part of the leading hemisphere of Tethys is dominated by a large impact crater called Odysseus, whose 450 km diameter is nearly 2/5 of that of Tethys itself.

Prior to the selection of Jezero, eight proposed landing sites for the mission were under consideration by September 2015; Columbia Hills in Gusev crater, Eberswalde crater, Holden crater, Jezero crater, Mawrth Vallis, Northeastern Syrtis Major Planum, Nili Fossae, and Southwestern Melas Chasma. A workshop was held on 8–10 February 2017 in Pasadena, California, to discuss these sites, with the goal of narrowing down the list to three sites for further consideration. The three sites chosen were Jezero crater, Northeastern Syrtis Major Planum, and Columbia Hills. Jezero crater was ultimately selected as the landing site in November 2018.

It has been proposed by some researchers that Ganges Mensa might be an extremely eroded version of one. Historically, other researchers have alternatively proposed that the modern shape of Ganges Mensa was a depositional and not erosional effect. The volcanic activity that formed Ganges Mensa could have occurred into a gigantic pingo-like laccolith composed of ice, or into a thoroughly-frozen lake within Ganges Chasma. Supporters of the subglacial volcanism origin hypothesis note that the Ganges Mensa's horizontally-oriented cap rock is morphologically consistent with the cap rock seen in tuyas in the Azas Plateau.

In 1987, Susan S. Nedell and David W. Andersen (San Jose State University) and Steven W. Squyres (NASA Ames Research Center) reported on the presence of layered deposits across Valles Marineris, offering the first detailed observations about the structure, stratigraphy, distribution and composition of the landforms within the valley network on Viking imagery. They focused particularly on deposits in Candor Chasma, making some regional generalizations. Nedell and her co-authors offered preliminary hypotheses as to how these deposits formed. The researchers concluded that a lacustrine depositional mechanism was generally the most probable formational hypothesis, against aeolian or explosively volcanic hypotheses.

In 2017, Selby Cull-Hearth and M. Caroline Clark (Bryn Mawr College) presented a comprehensive investigation of the mineralogy of Ganges Chasma using CRISM data. The authors reaffirmed the lower stratigraphic levels of the mesa as a mixture of monohydrated sulfates and ferric oxides. The deposits that host these spectral signatures on Ganges Mensa tend to contrast with surrounding terrain more darkly, and they appear to generally manifest in more unconsolidated deposits (including sand dunes on the surrounding valley floor). Olivine signatures, linear to the wall-floor boundary of Ganges Mensa, were observed by the researchers across the central edifice of the mesa.

This would have led to orbital eccentricity and tidal heating that may have warmed Tethys' interior enough to form a subsurface ocean. Subsequent freezing of the ocean after the moons escaped from the resonance may have generated the extensional stresses that created the enormous graben system of Ithaca Chasma on Tethys. The satellite system of Uranus is notably different from those of Jupiter and Saturn in that it lacks precise resonances among the larger moons, while the majority of the larger moons of Jupiter (3 of the 4 largest) and of Saturn (6 of the 8 largest) are in mean-motion resonances.

During the Voyager 2 flyby in 1986 the northern hemisphere of Ariel was not illuminated by the Sun because the spacecraft arrived during a southern solstice on Uranus. Nevertheless, because it was still illuminated by light reflected from Uranus, scientists using advanced processing methods were able to detect some details in the dark hemisphere. These analyses revealed a continuation of the Kachina Chasmata into the dark hemisphere, possibly as far as to the opposite limb. As the total length of the feature appears to be 1800–2200 km, it may be comparable to Ithaca Chasma on Tethys.

In 2008 and 2009 images retrieved by the VEx Venus Monitoring Camera using a near infrared one micron filter indicated several transient bright spots located in Ganis Chasma along the edges of the rift zone. In 2014, these transient bright spots were interpreted by Eugene Shalyin and his colleagues as possible active hotspot volcanism. Shalygin and his team created mosaics of the images of the study area and created maps of relative surface brightness. They interpreted these bright spots as hot matter at or just above the surface due to the result of a process that releases hot matter such as lava or gas (volcanism).

The mesa is separated from the canyon walls to the north by a moat- like stretch of valley floor, similar to Hebes and Capri Mensae and many of the mesa structures observed within Valles Marineris. Some researchers have interpreted Ganges Mensa to overlay chaos terrains in upstream Ganges Chasma. The mesa is surrounded by the most extensive and densely-concentrated dune sea on Mars outside the polar regions of the planet. A broad sandy plain stretches out to the south of the mesa and is interspersed with knobby plains and smaller mesas up to across in size, gradually decreasing in size to the east.

The highest plateau elevations on the Tharsis bulge occur in northern Syria Planum, western Noctis Labyrinthus, and the plains east of Arsia Mons. Between the northern and southern portions of the Tharsis bulge lies a relatively narrow, northeast-trending region that may be considered Tharsis proper or central Tharsis. It is defined by the three massive Tharsis Montes volcanoes (Arsia Mons, Pavonis Mons, and Ascraeus Mons), a number of smaller volcanic edifices, and adjacent plains consisting of young (mid to late Amazonian) lava flows. The lava plains slope gently to the east where they overlap and embay the older (Hesperian-aged) terrain of Echus Chasma and western Tempe Terra.

Animation of Tethys's rotation Pioneer 11 flew by Saturn in 1979, and its closest approach to Tethys was 329,197 km on 1 September 1979. One year later, on 12 November 1980, Voyager 1 flew 415,670 km from Tethys. Its twin spacecraft, Voyager 2, passed as close as 93,010 km from the moon on 26 August 1981. Although both spacecraft took images of Tethys, the resolution of Voyager 1's images did not exceed 15 km, and only those obtained by Voyager 2 had a resolution as high as 2 km. The first geological feature discovered in 1980 by Voyager 1 was Ithaca Chasma. Later in 1981 Voyager 2 revealed that it almost circled the moon running for 270°.

In December 1990, France's Commissariat à l'énergie atomique agreed to provide a commercial 900MW power plant, but plans did not materialize as France wanted Pakistan to provide entire financial funds for the plant. Furthermore, the U.S. Ambassador Robert Oakley further influenced on the project, showing growing concerns of the U.S. on the agreement. While talking to U.S. media, Nawaz Sharif declared that: "Pakistan possessed no [atomic] bomb... Pakistan would be happy to sign the Nuclear Nonproliferation Treaty (NPT) but it must be provided "first" to India to do the same". After France's project was cancelled, Nawaz Sharif successfully held talks with the China to build the largest commercial nuclear plant, CHASNUPP-I in Chasma city in Pakistan.

It extends from latitude 74.94°N to 82.2°N and from longitude 242.12°E to 300.77°E (59.23°W – 117.88°W). Its centre is located at latitude 81.6°N longitude 85.47°W. It marks the outer perimeter of Planum Boreum from longitude 242.12°E to 300.77°E, and it is formed by the eastern extension of the Olympia Cavi, a series of local troughs and depressions, which become longer and deeper as they merge to create the Rupes Tenuis scarp formation. The scarp is located to the west of Chasma Boreale, at the base of Planum Boreum, and its height varies from a few hundred metres to a maximum of approximately 1000 metres.

Siton Undae Spectral analysis of the dunes of the circumpolar ergs, including Siton Undae, using the OMEGA instrument on board the European Mars Express orbiter, indicates that 80 to 90 percent of these sands are composed of volcanic glass produced by eruptions of volcanoes situated in Martian glaciers. These ratios of glass and crystalline material are similar to those obtained in Iceland from eruptions of volcanoes below the ice. It is also theorised that significant amounts of granular glass may have been transferred to Vastitas Borealis, and Siton Undae, by catastrophic floods originating from Chryse Planitia, Valles Marineris, Juventae Chasma, and the southern Acidalia region of Mars. The dunes of Siton Undae contain amorphous silica-coated glass-rich sand.

However, the sulphur dioxide in the lower atmosphere remains stable. This could mean that a change in the global atmosphere caused the sulphur dioxide concentration to increase above the clouds. Even though the change in the atmosphere may be evidence that there have been volcanoes that erupted in Venus, it is difficult to determine whether they occurred or not. In March 2014, the first direct evidence for ongoing volcanism was located, in the form of infrared "flashes" over the edges of rift zone Ganis Chasma, near the shield volcano Sapas Mons. These flashes were detectable during two or three consequent Earth days in 2008 and 2009 and are thought to be caused either by hot gases or lava released from volcanic eruptions.

Atisha Naik is an Indian film actress has been in the field of acting since she was 8 years old when she made her debut in a Marathi play, Good Bye Doctor as a child artist. She made her film debut with Mahesh Manjrekar's Hindi film Pran Jaye Par Vachan Na Jaye. Recently, she played an important role of a lady, Sarpanch in the national award-winning film Deool. She has worked in Marathi serials like Aabhalmaya, Madhu Ithe Chandra Tithe, Dilya Ghari Tu Sukhi Raha, Ghadlay Bighadlay, Fu Baai Fu (Zee), Swapna Chya Palikadle, Ya Gojirwanya Gharaat, Ghadge and Soon (Colours Marathi) Bun Maska (Zee Yuva), Maansicha Chitrakaar Toh, Pudhcha Paaul etc.. She has also appeared in Hindi serials like Taarak Mehta Ka Ulta Chasma, Ek Packet Ummed etc.

Valles Marineris (Latin for Mariner Valleys, named after the Mariner 9 Mars orbiter of 1971–72 which discovered it) is a system of canyons that runs along the Martian surface east of the Tharsis region. At more than long, wide and up to deep, Valles Marineris is one of the largest canyons of the Solar System, surpassed in length only by the rift valleys of Earth. Valles Marineris is located along the equator of Mars, on the east side of the Tharsis Bulge, and stretches for nearly a quarter of the planet's circumference. The canyon system starts in the west with Noctis Labyrinthus; proceeding to the east are Tithonium and Ius chasmata, then Melas, Candor and Ophir chasmata, then Coprates Chasma, then Ganges, Capri and Eos chasmata; finally it empties into an outflow channel region containing chaotic terrain that ends in the basin of Chryse Planitia.

In 2006, Ross A. Beyer (NASA's Ames Research Center) submitted an abstract to the 37th Lunar and Planetary Sciences Conference reporting on his work characterizing in detail the aeolian morphologies present across the surface of Ganges Mensa. Beyer also investigated a crater off the eastern edge of the mesa which appears to demonstrate evidence of burial and later exhumation. The unveiled portions of that crater superpose a toe of the mesa, adding significant evidence to the hypothesis that Ganges Mensa was once a much more extensive landform that has since been greatly weathered. Beyer also submitted an abstract to the American Geophysical Union meeting that year to report on the relationship of light- toned mound deposits in Ganges Chasma to the basal unit of Ganges Mensa, using OMEGA spectral data to note similarities in kieserite signatures between the sulfate-bearing mesa layers and those mounds.

There were buildings of historic significance in the city, now largely demolished but a few of which still exist, such as a well (chasma baoli) built by Chaudry Balik Ram Jugga, and the shrine of Syed Nathey Shah Gardezi& Dhkou Tahseel, pipal, pakka, faddah, and thana bazaar are situated in the old part of the city while Quaid e Azam, Multan, and Allama Iqbal Roads, Model Town, Rehman Town and Qazi town are examples of recent expansion. The first modern area was developed in the 1960s for meeting the housing needs of the Gamon company's European workers and engineers; this area is now Mailsi Garrison, housing Pakistan's army defence units. There were two cotton ginning factories in Mailsi prior to independence; the increase in cultivated area resulted in high production of cotton which led to establishment of cotton ginning factories and oil mills. In the city of Mailsi there are many towns, including Madina Town and Fadaa Town.

At that area, some of the dunes exhibit dark streaks that may have been caused by katabatic winds. This may indicate sand movement, due to Aeolian activity, which is recent enough to retain the streaks, otherwise these marks tend to disappear with time; other dunes do not exhibit such marks. The dunes of Hyperboreae Undae, according to data provided by the Compact Reconnaissance Imaging Spectrometer for Mars, exhibit the weakest signature for the presence of surface ice in the area of Chasma Boreale. Hyperboreae Undae, along with Abalos and Siton Undae, contributes sand to mainly medium-density dune fields east of Olympia Undae and extending to the Martian prime meridian, Image analysis research, using the method of spectral derivatives, has indicated that Hyperboreae Undae, as well as the other dense officially-named northern circumpolar dune fields (Olympia Undae, Abalos Undae, and Siton Undae), show the highest density of gypsum in the area.

In 2008, Matthew Chojnacki and Jeffrey E. Moersch of the University of Tennessee presented a poster at the American Geophysical Union Fall Meeting to report on their work characterizing the ergs of Valles Marineris using moderate- to high-resolution THEMIS, CTX, and HiRISE data. Among other results, the authors asserted that the highest concentrations of dunes within Valles Marineris—including the largest non- polar erg on Mars—can be found within Ganges Chasma immediately surrounding Ganges Mensa. In 2008, Mariam Sowe, Ernst Hauber and Ralf Jaumann (German Aerospace Center, or DLR), John F. Mustard and Leah H. Roach (Brown University), and Gerhard Neukum (Free University of Berlin) submitted an abstract to the European Planetary Science Congress to report an analysis of the composition of the interior layered deposits within Ganges Mensa using CRISM (spectral), THEMIS (day/night thermophysical), and HRSC (elevation) data. The researchers found spectral signatures on Ganges Mensa supportive of a saline lacustrine origin, owing largely to the likely presence of polyhydrated sulfates such as kieserite.