The other, Rimae Theaetetus, has a length of 16 miles (25 km).
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Rimae Secchi (with southern part cropped). Photo by Apollo 11, 1969. LRO, 2018. Rimae Secchi is a system of rilles on the Moon, in northwestern Mare Fecunditatis.
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Another rille system lies to the south, designated Rimae Ramsden.
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Rimae Sirsalis is a lunar rille. It is located at and is 426 km long. It was formed by extension of the surface, possibly due to dike propagation in the subsurface. Rimae Sirsalis cuts across highlands almost exclusively.
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The southern rim is almost contacting a rille system named the Rimae Plinius.
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The lunar features Promontorium Fresnel and Rimae Fresnel were later named after him.
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Other rille systems lie in the vicinity, including the Rimae Ritter to the southeast and Rimae Sosigenes to the northeast. The crater was named after Philip III of Macedon (Arrhidaeus).Antonín Rükl, Atlas of the Moon (Hamlyn, 1991), p. 96.
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The rille system to the north of the crater is designated Rimae Maclear, while the rilles to the south-southwest are named Rimae Sosigenes. The Rimae Maclear stretches for about 100 kilometers, reaching Al-Bakri to the north along the edge of the mare. It is named after Sir Thomas Maclear, Her Majesty's astronomer at the Royal Observatory, Cape of Good Hope (Cape Town, South Africa), from 1833 to 1870.
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This crater is roughly circular and bowl-shaped, with an interior that has a higher albedo than the surrounding terrain. It lies in a region that has a number of rille systems, with the Rimae Hippalus to the northwest, and the Rimae Ramsden to the south and east.
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Rimae Fresnel are the series of northeast-trending graben shown in this image Rimae Fresnel is a 90km-long arcuate escarpment on the Moon at . Both the escarpment and the nearby Promontorium Fresnel were named after the French physicist Augustin-Jean Fresnel. Accessed December 19, 2017"Fresnel summary". August 2002.
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To the west is a rille system designated the Rimae Bürg, which spans a distance of about 100 kilometers.
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There is a small rise at the midpoint. Recent deposits of highland material have been observed within the crater interior. Rimae Sulpicius Gallus To the northwest is a rille system designated the Rimae Sulpicius Gallus. These extend to the northwest for a distance of about 90 kilometers, curving and branching out to follow the edge of the mare.
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Oblique image also from Apollo 16 Most of the Rimae Herigonius and Herigonius K crater (below center). The rimae (rilles) extend to the south out of the picture. Herigonius is a small lunar impact crater that is located in the southern part of the Oceanus Procellarum, to the northeast of the crater Gassendi. It was named after French mathematician and astronomer Pierre Hérigone.
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The northern system is designated Rimae Maclear, after the crater Maclear just to the east of the bay. At the southern end of the bay entrance is the Rimae Sosigenes, named for the crater Sosigenes to the south. At the west end of the bay is a finger of mare surface that extends to the northwest for almost 100 km.
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In the mare to the south are several rises collectively named the Montes Teneriffe. To the north lies the wide stretch of the Mare Frigoris. East of the crater, among the Montes Alpes, are several rilles collectively named the Rimae Plato. Rimae Plato (Lunar Orbiter 4 image) The age of Plato is about 3.84 billion years, only slightly younger than the Mare Imbrium to the south.
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To the east is a rille system named the Rimae Sirsalis. The longest of these rilles follows a line running approximately north-northeast to south-southwest, just clearing the southeastern rim of Sirsalis by about 10 kilometers. This long rille runs 330 kilometers from the shore of Oceanus Procellarum until it crosses the crater Darwin A and intersects the Rimae Darwin to the east of Darwin.
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A rille from the Rimae Repsold system crosses the northeastern rim and traverses the interior, forking near the midpoint to continue towards the west-southwest and the south.
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100 km farther to the west the craters Menelaus and Auwers are embedded within the range, and to their northeast are the Rimae Menelaus. Where the mountain range curves up to the northwest, the cup-shaped crater Sulpicius Gallus lies nearby on the lunar mare. Just to the northwest of this crater, and paralleling the mountains, are the Rimae Sulpicius Gallus. Several small "lakes", formed from basaltic lava, lie along the southwest face of the range.
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Lunar Orbiter 4 image of Daniell (note different lighting than above) Apollo 15 image Lunar Orbiter 4 image of Rimae Daniell Daniell is a lunar impact crater located in the southern half of the Lacus Somniorum. To the south- southeast is the much larger crater Posidonius. The Rimae Daniell rille system are to the west of Daniell crater. The rim of Daniell is oval in form, with the long axis oriented north-northwest to south-southeast.
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The main-belt asteroid 4279 De Gasparis as well as the 30-kilometer lunar crater de Gasparis and the nearby 93-kilometer long fracture Rimae de Gasparis, are named in his honour.
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The feature lies to the southwest of Mare Nubium, and southeast of Mare Humorum. This mare is notable for a system of rilles in the western end named the Rimae Ramsden, and for the wide Rima Hesiodus that extends from near the midpoint to the east-northeast roughly 300 km. The flooded crater Capuanus occupies the southern center of the Palus Epidemiarum, and is attached to the southern edge. Near the western end is the flooded crater Ramsden, after which the Rimae Ramsden are named.
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South of the crater are the rilles of the Rimae Maclear. Al-Bakri was designated Tacquet A prior to being assigned a name by the IAU. The tiny Tacquet lies to the northwest on the Mare Serenitatis.
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The lunar crater Hypatia was also named for her, in addition to craters named for her father Theon. The 180 km Rimae Hypatia are located north of the crater, one degree south of the equator, along the Mare Tranquillitatis.
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Rimae Ariadaeus from Apollo 10. NASA photo. This crater marks the eastern extent of the rille designated Rima Ariadaeus. This wide rille extends in a nearly straight line to the west- northwest, passing just to the north of the crater Silberschlag.
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On the flood are a pair of low-rimmed craters that are joined at the rims and span most of the central Cavendish crater floor from east to west. A rille from the Rimae de Gasparis reaches the eastern rim of Cavendish.
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The flooded floor is irregular and uneven, and contains a system of faint rilles called the Rimae Charocnac. There is no central peak, and no trace of a ray system. The ground around the crater is rugged, with a hilly, sloping rampart to the west.
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To the north of Capuanus is the western extreme of the wide rille named Rima Hesiodus, which runs to the east-northeast. To the west- northwest is the crater Ramsden, and between Capuanus and Ramsden lies a system of intersecting rilles named the Rimae Ramsden.
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It has a minor ray system that extends for a distance of 130 kilometers. There is a group of rilles located to the west of the crater named the Rimae Bode. Its name comes from the tap on Bode Faleti discovered in 2011 in Chicago, Illinois.
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To the northwest of Ritter is a system of parallel rilles designated Rimae Ritter. These follow a course to the northwest. Ranger 8 flew over Ritter prior to impact in Mare Tranquilitatis. Both Sabine and Ritter were originally believed to be calderas rather than impact craters.
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There is a small break in the eastern wall. On the mare to the south of the patch of highland containing Lubbock is the rille system designated Rimae Goclenius. The parallel rays from the crater pair of Messier and Messier A reaches the rim of Lubbock H to the north.
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Just to the north is a system of rilles named the Rimae Plinius and touching it is the Brackett crater which is more than a crater diameter north. At the northwest edge of the rille is the Promontorium Archerusia, a cape off the western rim that encloses the Mare Serenitatis.
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The floor has been flooded by lava in the past, leaving a relatively flat surface that is broken by a series of narrow clefts. These are collectively designated the Rimae Parry. The clefts cross the rim to the south and also to the north, extending into the neighboring Fra Mauro.
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Tacquet is a small, bowl-shaped crater that lies near the southern edge of Mare Serenitatis, in the northeast part of the Moon. The surface near the crater is marked by high-albedo ejecta. To the west is a system of rilles designated the Rimae Menelaus. Its diameter is 6.4 km.
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The surviving outer rim is not especially circular, having been reshaped into a somewhat pentagonal outline. There are deep gouges from cratering along the northeastern rim. The interior floor is not in much better shape, being rough and irregular. To the northeast of this crater is a system of rilles designated Rimae Maupertuis.
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The rilles are centered at . The northern part of Rimae Secchi is surrounded with a dark halo, probably pyroclastic deposits like volcanic ash. Such deposits are common near the edges of lunar maria, including several areas in Mare Fecunditatis. To see this feature, a telescope with an aperture of 20 cm or larger is needed.
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Hase A is a small crater that lies in the interior of Hase, near the irregular northern rim. The remainder of the floor is rough and irregular. To the southeast of Hase D is a system of linear rilles designated Rimae Hase. Their north-western extension transects western part of Hase and Hase D.
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To the east of the crater on the surface and edges of the Mare Humorum is a rille system designated Rimae Mersenius. These rilles are generally parallel and run to the north-northeast for a length of about 230 kilometers. The crater is named after the 17th-century French philosopher and physicist Marin Mersenne.
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The rim of this crater has been opened in the northern and southern ends, leaving two curved ridges facing each other across the crater floor. To the south is a pair of rilles designated the Rimae Secchi. These lie near the edge of the mare, and have a combined length of about 40 kilometers.
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The crater rim has a high albedo, making it relatively bright. It has a small central rise at the midpoint of the floor. To the east on the mare is a formation of parallel rilles designated the Rimae Sosigenes. These follow a course to the north, and have a length of about 150 kilometers.
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The rim is somewhat oval and irregular in outline, with depressions at the north and south walls. It has a slight rampart, but lacks terraces, a central peak, or a ray system. The crater lies directly across a rille system named the Rimae Ramsden. These span an area 130 kilometers across, sprawling over the western Palus Epidemiarum.
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About 70 kilometers to the north of Hypatia is a system of linear rilles designated Rimae Hypatia, running about 180 kilometers across the Mare Tranquillitatis, and generally following a course to the south-southeast. The part of the rilles close to the crater Moltke was informally called U.S. Highway 1 by the Apollo 10 and Apollo 11 crews.
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The floor is relatively flat, except for some irregularities in the southwestern quadrant of the crater. There is a rille system named the Rimae Arzachel that runs from the northern wall to the southeast rim. A small crater lies prominently in the floor to the east of the central peak, with a pair of smaller craterlets located nearby.
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Oblique view of Römer from Apollo 17. Apollo 15 captured this view as it flew over Römer at low altitude. Lunar Orbiter 4 image of Rimae Römer Römer is a lunar impact crater that is located to the north of the Sinus Amoris in the northeast section of the Moon. It was named after Danish astronomer Ole Rømer.
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To the southeast is the somewhat larger Krieger. There are several small rilles to the southwest of Wollaston, forming part of the Rimae Prinz. This is a circular, cup-shaped crater with a higher albedo than the surrounding mare. It has a raised rim that is free from impact erosion, and is surrounded by a small radial skirt of ejecta.
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Two mountains within a highland mass informally called "The Helmet" (by the Apollo 16 crew) are informally named Herigonius Eta (η) and Herigonius Pi (π). Eta is the larger mountain on the northern edge of the Helmet, and Pi is along the southwest edge. North and northwest of the crater is the wrinkle ridge Dorsa Ewing, which also contacts Rimae Herigonius.
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Image of Lacus Mortis featuring rilles (narrow depressions collectively called Rimae Bürg) thought to represent lava tubes beneath the surface, may be explored by the Asagumo lunar rover during Spacebit Mission One.3D Printed structure of Lacus Mortis pit crater with assumption of a cave underneath. Ik-Seon Hong, Eunjin Cho, Yu Yi, Jaehyung Yu, Junichi Haruyama. 2nd International Planetary Caves Conference (2015).
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Cauchy lies between the Rupes Cauchy and the Rimae Cauchy, as described below. South of Rupes Cauchy are two lunar domes designated Omega (ω) Cauchy and Tau (τ) Cauchy. They lie to the south and southwest of Cauchy respectively. Each lunar dome has a small depression at its crest, which is likely to be a volcanic vent rather than an impact crater.
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LRO image Promontorium Fresnel (Latin for "Cape Fresnel") is a headland on the near side of the Moon. It is located at the northern end of the Montes Apenninus and separates the lunar mares of Mare Serenitatis and Mare Imbrium. Just west of the mountainous cape is Rimae Fresnel. Both features were named after the French physicist Augustin-Jean Fresnel.
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Adams is a lunar impact crater that is located in the rugged southeastern section of the Moon, near the lunar limb. It lies just to the southwest of the crater Legendre. To the northwest are the craters Hase and Petavius, and to the southwest is Furnerius. To the southwest of Adams is a system of rilles designated the Rimae Hase.
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Only a low, eroded rim of Hevelius rises above the surface. The western wall is overlain by several small impacts. The flat floor of the crater has been flooded by lava, and is now cross-crossed by a system of small clefts named the Rimae Hevelius. There is a low, one-km-high central peak offset to the northwest of the midpoint.
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The floor has the same low albedo as the nearby mare, giving it a dark appearance. It is marked by a pair of tiny craterlets near the northeast and northwest interior walls. A slender rille crosses the crater floor from north to south, passing to the east of the central peak. To the west of Campanus is the rille system named Rimae Hippalus.
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High-resolution view from Lunar Orbiter 5 Moltke is a lunar impact crater near the southern edge of the Mare Tranquillitatis. It is a small, bowl-shaped crater surrounded by a bright halo of higher-albedo material. Just to the south lies the rille system named Rimae Hypatia. These follow a course running roughly east-southeast to west-northwest, and have a length of approximately 180 kilometers.
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Another view from Apollo 17 Ching-Te is a small lunar impact crater located in a mountainous area to the east of the Mare Serenitatis. It is a circular, bowl-shaped formation with no distinguishing features. To the south-southeast is the crater Fabbroni, and to the northeast is Littrow. North of Ching-Te is the Rimae Littrow rille system as well as the crater Clerke.
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Marth is a small lunar impact crater located in the northwest part of the Palus Epidemiarum. It was named after German astronomer Albert Marth. To the northwest is the crater Dunthorne, and to the southwest lies Ramsden. This feature lies in a system of rilles named the Rimae Ramsden, and an interrupted branch passes only a few kilometers to the south of the rim.
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Oblique view from Apollo 15 Väisälä is a tiny lunar impact crater located on a rise in the Oceanus Procellarum. Sharing the same continental island are the brilliant crater Aristarchus to the south-southeast and Herodotus to the south-southwest. Väisälä lies just to the west of the Rupes Toscanelli fault line, and the Rimae Aristarchus rille system. To the southwest is the notable Vallis Schröteri cleft.
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The crater Cichus forms the eastern end of the mare. The northern extension of the mare reaches the outer rims of the crater pair Campanus and Mercator. A narrow valley between these craters joins Palus Epidemiarum with Mare Nubium, and a rille from the Rimae Ramsden follows the course of this cleft. The small double-walled crater Marth lies at the southern midpoint of this northern extension.
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They are approximately 40 km long and run along the shore of the mare. Rimae Secchi are named after the nearby crater Secchi which, in turn, is named after an Italian astronomer Angelo Secchi. The name of the rilles was approved by the International Astronomical Union in 1985. In 1974, the name Fossae Secchi was proposed on a mapLunar Topographic Orthophotomap LTO-61C4 (Secchi).
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There is also a system of rilles that criss-crosses the floor, named the Rimae Gassendi. The fresh crater Gassendi A is adjacent to Gassendi to the north. Due to its ray system, Gassendi A is mapped as part of the Copernican System.The geologic history of the Moon, 1987, Wilhelms, Don E.; with sections by McCauley, John F.; Trask, Newell J. USGS Professional Paper: 1348.
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This surface is broken across the northeast by a pair of clefts that form a part of the Rimae Goclenius. These extend northwest from the Goclenius region. The central rise of Gutenberg is a semi-circular range of hills that are the most prominent in the south, and the concave part lies open to the east. The floor is otherwise not marred by any significant craters.
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Zupus is the lava-flooded remains of a lunar impact crater. It is located on a southwestern reach of the Oceanus Procellarum, to the northwest of Mare Humorum. To the north-northeast is the flooded crater Billy, and some distance to the southeast is Mersenius. A system of faint rilles named the Rimae Zupus lie to the northwest, following a course to the north-northwest towards the mare.
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This crater has been heavily damaged by impacts and much of the rim has disintegrated, leaving a rugged region of small craters. The most intact section of the rim is in the southeastern part, which separates this formation from the adjacent mare. The satellite crater Repsold G overlies the southwestern part of the crater. The interior floor of Repsold contains a system of rilles named the Rimae Repsold.
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The rim of Parry is heavily worn and slightly distorted due to the co-joined formations. The wall is the most prominent along the northwest, and crossed along the southwest by the small Parry B. The floor has been flooded by lava, and is relatively flat. At the midpoint is a pair of small craters. A rille system, called the Rimae Parry, crosses the region in a series of graben.
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Lepaute is a small lunar impact crater that is located along the western edge of the Palus Epidemiarum, a minor lunar mare in the southwestern part of the Moon's near side. It was named after French astronomer Nicole-Reine Lepaute. To the east is the larger crater Ramsden, within a system of rilles named the Rimae Ramsden. This is an elongated crater feature that is longer in the north–south direction.
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Boscovich is a lunar impact crater that has been almost completely eroded away by subsequent impacts. It is located west-northwest of the crater Julius Caesar, and south-southeast of the prominent Manilius. The crater floor has a low albedo, and the dark hue makes it relatively easy to recognize. The surface is crossed by the rille system designated Rimae Boscovich that extends for a diameter of 40 kilometres.
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Oblique view from Apollo 15, showing the bright rays Another view from Apollo 15 Detail of the interior from Lunar Orbiter 5 Dionysius is a lunar impact crater that lies on the western edge of the Mare Tranquillitatis. It was named after Dionysius the Areopagite. To the southeast is the crater pair of Ritter and Sabine. Just to the northwest is the system of rilles designated Rimae Ritter.
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Apollo 16 image Oblique view from Apollo 11 Goclenius is a lunar impact crater that is located near the west edge of Mare Fecunditatis. It lies to the southeast of the lava-flooded crater Gutenberg, and north of Magelhaens. To the northwest is a parallel rille system that follow a course toward the northwest, running for a length of up to 240 kilometers. This feature is named the Rimae Goclenius.
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The surviving rim is worn and eroded, forming a low, circular mountain range. The lava-flooded floor of Hippalus is bisected by a wide rille belonging to the Rimae Hippalus. This rille follows a course to the south before curving gently to the southwest for a total length of 240 kilometers. The crater floor to the east of this rille is more rugged than the area in the western half.
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The eastern edge of Palus Epidemiarum reaches the west rim of Mercator, and a rille from the Rimae Ramsden reaches the western rim at the site of the craterlet Mercator C. The rim of Mercator is only somewhat eroded, and several tiny craterlets lie on the west and eastern rims. The interior floor has been flooded by lava in the past, leaving a relatively smooth and featureless surface.
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Herigonius is roughly circular, with an inward bulge and narrower inner wall along the northeast. In the interior of the sloping inner walls is a floor about half the diameter of the crater. About 60 kilometers to the west of Herigonius is a sinuous rille designated Rimae Herigonius. This cleft is about 100 kilometers in length and runs generally in a north-south direction, while curving to the east at the north end.
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Apollo 15 image Oblique close up of the northwest crater wall, from Apollo 15 Menelaus () is a young lunar impact crater located on the southern shore of Mare Serenitatis near the eastern end of the Montes Hæmus mountain range. Its diameter is 27 km. To the southwest is the small crater Auwers, and to the west-southwest is the even smaller Daubrée. To the northeast is a faint rille system named the Rimae Menelaus.
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The small, cup-shaped crater Liebig A lies along the inner wall and part of the interior floor. The western edge of the Mare Humorum is a fault line designated the Rupes Liebig, named after this crater. This fault extends for about 180 km along the shore. To the southwest, in the section of lava-flooded surface between Liebig and de Gasparis, is a system of rilles named the Rimae de Gasparis.
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Finally the lake curves back to the south, joining a region of rough terrain along the northern border of the Mare Serenitatis. In the southern half of this border area lies a rille system designated the Rimae Daniell. These were named for the crater Daniell, a small formation north of Posidonius that is encircled by the Lacus Somniorum. To the north of Daniell, near the northern edge of this feature, lies the small crater Grove.
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Fontana is a lunar impact crater that is located in the southwestern part of the Moon's near side, to the south of the Oceanus Procellarum. It lies to the west-northwest of the flooded crater Zupus. Midway between Fontana and Zupus is a rille system designated Rimae Zupus. This is a low-rimmed crater with an interior floor that is marked only by several small craterlets, and a few low ridges in the southwest.
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The formation is symmetric, with a light-hued outer rim and a darker interior floor. A rille belonging to the Rimae Parry almost connects with the north-northwestern rim of Tolansky. It was named after British physicist Samuel Tolansky.Tolansky, Gazetteer of Planetary Nomenclature, International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN) It was formerly known as Parry A, prior to its current name being approved by the IAU in 1976.
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Closeup of the Rimae Hevelius at low sun angle, in the northeast portion of the crater floor. From Lunar Orbiter 3 Hevelius is a low-rimmed lunar impact crater that lies at the western edge of the Oceanus Procellarum, named after the astronomer Johannes Hevelius. The smaller but prominent crater Cavalerius is joined to the northern rim by low ridges. Due south of Hevelius is the crater Lohrmann and the dark-hued Grimaldi.
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This is a floor-fractured crater with a rough and hilly interior that has a lighter albedo than the surroundings. Floor- fractures are usually created as a result of volcanic modifications. There are two dark patches along the inner edge of the walls; one along the north edge and another besides the southeast edges. A system of slender clefts named the Rimae Atlas crosses the crater floor, and were created by volcanism.
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This crater is notable for the formation of rilles that criss-cross the floor and the surrounding surface. This system of clefts in the surface is designated Rimae de Gasparis, and they span an area of about 130 kilometers in diameter. The rilles are thought to have been created due to tectonic faults deep below the surface. As they cut across de Gasparis, this indicates that they were formed after the crater.
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The northern half of the rim has outward bulges to the northeast, north, and northwest. The interior floor is rough in places, with several small and tiny craters along the floor and the eastern rim. To the northwest of this formation is the unusual Gerard Q Inner (eastern floor covered in dark-hued basaltic lava) within the larger Gerard Q Outer, and a system of rilles named the Rimae Gerard. These extend for a distance of about 100 kilometers.
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The rim has a wide break at the northern end and several smaller breaks to the south and southeast. The satellite crater Opelt E lies at the southern end of the surviving western rim. The interior floor is nearly level, with the exception of a slight rise to the southwest, which is continuous with a wrinkle ridge to the south. To the north of Opelt on the lunar mare is a sinuous system of rilles designated Rimae Opelt.
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The interior floor is irregular and complex, with a series of ridges and small clefts (similar to Vitello). The crater is concentric with a larger, older crater designated Damoiseau MDamoiseau M, Gazetteer of Planetary Nomenclature International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN) that is approximately twice the diameter. This outer feature is missing a rim to the northeast where it intersects the lunar mare. To the southeast is a rille system named the Rimae Grimaldi.
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De Vico is a small lunar impact crater that is located in the southwest part of the Moon, to the south of the crater Sirsalis. To the west-northwest is Crüger. De Vico is a circular, bowl-shaped formation with a small, flat bottom at the midpoint. To the northwest is the lava-flooded remains of De Vico T. Beyond is a linear rille designated Rimae Sirsalis that follows a path to the northeast past the rim of Sirsalis.
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This minor planet was named after Johannes Gutenberg (ca. 1400–1468), a German inventor who started the Printing Revolution with the introduction of mechanical movable type printing. Gutenberg lived and died in Mainz and the neighboring Eltville am Rhein. The was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (). The crater Gutenberg on the Moon and the feature Rimae Gutenberg, a 223-kilometer long groove near the crater, were also named after him.
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Apollo 15 image Toscanelli is a tiny, bowl-shaped lunar impact crater that is located to the north of the prominent crater Aristarchus, in the northwestern part of the Moon. The crater lies at the southern end of a rille that proceeds towards the north. This rille is part of a nearby system that has the designation Rimae Aristarchus. Just to the south of Toscanelli is a fault line in the surface named the Rupes Toscanelli, after the crater.
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Detail of part of Hadley Rille Rille (German for 'groove') is typically used to describe any of the long, narrow depressions in the surface of the Moon that resemble channels. The Latin term is rima, plural rimae. Typically a rille can be up to several kilometers wide and hundreds of kilometers in length. However, the term has also been used loosely to describe similar structures on a number of planets in the Solar System, including Mars, Venus, and on a number of moons.
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But he assigned this name (in the form Mons Æmus) to another feature – remains of the rim of crater Alexander, located on the other side of Mare Serenitatis. Later the name moved to the subject of this article. The same name, but with reversed order of words – Haemus Montes – belongs to one of mountain systems on Io. Several rille systems lie along the eastern side of this range. The eastern end of the range forms the western terminus of a rille system designated Rimae Plinius.
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Location of the Aristarchus crater on the Moon. Aristarchus is located on an elevated rocky rise, known as the Aristarchus Plateau, in the midst of the Oceanus Procellarum, a large expanse of lunar mare. This is a tilted crustal block, about 200 km across, that rises to a maximum elevation of 2 km above the mare in the southeastern section. Aristarchus is just to the east of the crater Herodotus and the Vallis Schröteri, and south of a system of narrow sinuous rilles named Rimae Aristarchus.
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Römer has a ray system, and due to these rays, it is mapped as part of the Copernican System.The geologic history of the Moon, 1987, Wilhelms, Don E.; with sections by McCauley, John F.; Trask, Newell J. USGS Professional Paper: 1348. Plate 11: Copernican System (online) To the northwest of the crater is a prominent system of rilles named the Rimae Römer. These follow a course to the north from the western rim of the crater, and have a combined length of about 110 kilometres.
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Oblique Apollo 12 image Apollo 16 image at high sun angle Leakey is a small, undistinguished lunar impact crater that is located in an area of rough terrain in the eastern part of the Moon. It was named after British archaeologist Louis Leakey. The immediate area is not notable for crater features, although some distance to the southwest is the crater pair of Capella and Isidorus. In the surface between this pair and Leakey is a system of rilles designated the Rimae Gutenberg that follow a course to the southeast.
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The rim of Posidonius is shallow and obscured, especially on the western edge, and the interior has been overlain by a lava flow in the past. The crater ramparts can still be observed to the south and east of the crater rim, and to a lesser degree to the north. There is a smaller, semi-circular rim of a concentric, flooded crater within the main rim, offset towards the eastern edge. There is no central peak, but the floor is hilly and laced with a rille system named the Rimae Posidonius.
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To the northwest of Santos-Dumont is a 90-km-wide system of rilles designated the Rimae Fresnel, being named for the Promontorium Fresnel that lies to the north of the crater. This last formation forms the northern end of the Montes Apenninus, and lies astride the gap that joins the Mare Imbrium to the west with the Mare Serenitatis to the east. To the southeast, in the valley past Mons Hadley, is the landing site of the Apollo 15 mission. This feature is named in honour of the Brazilian aviation pioneer Alberto Santos-Dumont.
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The northern and southern parts of the rim of Vasco da Gama have been heavily eroded by impacts, with the western and eastern rims being more intact. The smaller crater Vasco da Gama S intrudes into the southeastern rim, and just to its southwest is Vasco da Gama T. Near the northeastern rim is Vasco da Gama B. There is a low central massif near the midpoint of the interior. The interior floor of satellite crater Vasco da Gama R contains a system of rilles designated the Rimae Vasco da Gama.
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The rim of this crater is worn, distorted and irregular, having a somewhat egg-like outline. The crater floor has been covered in lava, and a rille cuts across the floor towards the northwest, in the same direction as the other members of the Rimae Goclenius. A similar rille lies across the floor of Gutenberg, and it is likely that these features were all formed at the same time, after the original craters were created. There is a low central rise located to the northwest of the crater's midpoint.
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Just to the southwest of Palmieri is the small crater Palmieri E. The interior floor of Palmieri has been flooded by lava, leaving a dark interior surface that has a similar albedo to the lunar mare to the northeast. This floor is joined with a long expanse of lava surface to the north of Palmieri that proceeds northwards until it reaches the area between Liebig and de Gasparis. The floor is marked by a system of rilles named the Rimae Palmieri that continue to the north and southeast beyond the crater perimeter. These narrow rifts extend for about 150 kilometers.
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Oblique Apollo 17 image of Clerke Granular debris flows within Clerke Clerke is a tiny lunar impact crater named after Irish astronomer Agnes Mary Clerke, who played a role in bringing astronomy and astrophysics to the public in Victorian England.LROC: Clerke Crater It is located near the eastern edge of Mare Serenitatis in the midst of a rille system named the Rimae Littrow after the crater Littrow to the east. It is roughly circular and cup-shaped, with a relatively high albedo. In a valley to the southeast is the landing site of the Apollo 17 mission.
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Riccioli is older than the Orientale basin to the southwest because the ejecta from the impact that created the Orientale basin overlies the crater. This debris lies in ridges that regionally trend northeast-southwest, but trend in a direction parallel to Riccioli's northeast wall in that part of the crater. A system of rilles named the Rimae Riccioli lies across the interior, and crosscut the ejecta ridges. In the northern half of the interior, the dark covering of lava that resurfaced the floor is visible, and apparently covers some of the ejecta ridges and floods some of the rilles.
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Apollo 11 image of Rimae Gutenberg, facing southeast. The rim of Gutenberg is worn and eroded, most notably in the east where it is broken by the overlapping crater Gutenberg E. This crater in turn has gaps in its southeast and southwest rims, forming a passage to the lunar mare to the east. There are also clefts and valleys in the southern rim where it joins Gutenberg C. The crater Gutenberg A intrudes into the southwest rim. The floors of Gutenberg and Gutenberg E have been flooded in the past by lava, forming a relatively flat plain across the bottom.
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