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Odin Formation
The Caloris group is a set of geologic units on Mercury. McCauley and othersMcCauley, J. F., Guest, J. E., Schaber, G. G., Trask, N. J., and Greeley, Ronald, 1980, Stratigraphy of the Caloris Basin, Mercury: Icarus, 1980 have proposed the name “Caloris Group” to include the mappable units created by the impact that formed the Caloris Basin and have formally named four formations within the group, which were first recognized and named informally by Trask and Guest. Like the Imbrium and Orientale Basins on the Moon, Caloris Basin is surrounded by an extensive and well-preserved ejecta blanket As on the Moon, where ejecta from the better preserved basins was used to construct a stratigraphy, the ejecta from the Caloris Basin also can be used as a marker horizon. This ejecta is recognizable to a distance of about one basin diameter in the Tolstoj quadrangle and the adjacent Shakespeare quadrangle to the north. Undoubtedly, the ejecta also influences a large part of the terrain to ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mercury (planet)
Mercury is the smallest planet in the Solar System and the closest to the Sun. Its orbit around the Sun takes 87.97 Earth days, the shortest of all the Sun's planets. It is named after the Roman god ' ( Mercury), god of commerce, messenger of the gods, and mediator between gods and mortals, corresponding to the Greek god Hermes (). Like Venus, Mercury orbits the Sun within Earth's orbit as an inferior planet, and its apparent distance from the Sun as viewed from Earth never exceeds 28°. This proximity to the Sun means the planet can only be seen near the western horizon after sunset or the eastern horizon before sunrise, usually in twilight. At this time, it may appear as a bright star-like object, but is more difficult to observe than Venus. From Earth, the planet telescopically displays the complete range of phases, similar to Venus and the Moon, which recurs over its synodic period of approximately 116 days. The synodic proximity of Mercury to Earth makes Mercury most ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Serenitatis Basin
Mare Serenitatis (Latin ''serēnitātis'', the "Sea of Serenity") is a lunar mare located to the east of Mare Imbrium on the Moon. Its diameter is . Geology Mare Serenitatis is located within the Serenitatis basin, which is of the Nectarian epoch. The material surrounding the mare is of the Lower Imbrian epoch, while the mare material is of the Upper Imbrian epoch. The mare basalt covers a majority of the basin and overflows into Lacus Somniorum to the northeast. The most noticeable feature is the crater Posidonius on the northeast rim of the mare. The ring feature to the west of the mare is indistinct, except for Montes Haemus. Mare Serenitatis connects with Mare Tranquillitatis to the southeast and borders Mare Vaporum to the southwest. Mare Serenitatis is an example of a mascon, an anomalous gravitational region on the moon. A mass concentration (mascon), or gravitational high, was identified in the center of Mare Serenitatis from Doppler tracking of the five Lunar Orbiter ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Fra Mauro Formation
The Fra Mauro formation (or Fra Mauro Highlands) is a formation on the near side of Earth's Moon that served as the landing site for the American Apollo 14 mission in 1971. It is named after the 80-kilometer-diameter crater Fra Mauro, located within it. The formation, as well as Fra Mauro crater, take their names from a 15th-century Italian monk and mapmaker of the same name. Apollo 13 was originally scheduled to land in the Fra Mauro highlands, but was unable due to an in-flight technical failure. Fra Mauro is thought to have been formed from ejecta, or debris, from the impact which formed Mare Imbrium. During Apollo 14, the crew members sampled ejecta from Cone crater, a feature close in proximity to the immediate landing site of the mission, which provided insight into the composition of material deep inside the formation. Data from the mission has helped to determine the approximate age of Mare Imbrium, suggesting that it is no more than about 4.25 billion years old. Form ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Van Eyck (crater)
Van Eyck is a 271 km diameter impact basin in the Shakespeare quadrangle of Mercury. It is located at 43.22°N, 159.43°W and is named after the 15th century Flemish painter Jan van Eyck. Its name was adopted by the International Astronomical Union (IAU) in 1979. Van Eyck lies on the southwestern margin of the even-larger Shakespeare basin. The younger Mansur Mansour ( ar, منصور, Manṣūr); also spelled Mounsor, Monsur (Bengali), Mansoor, Manser, Mansur, Mansyur (Indonesian) or Mensur (Turkish), is a male Arabic name that means "He who is victorious", from the Arabic root '' naṣr'' (نصر), m ... crater lies to the northwest of Van Eyck. References Impact craters on Mercury Jan van Eyck {{crater-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Odin Planitia
Odin Planitia is a large basin on Mercury located at 23.3° N, 171.6° W. It was named after the Norse god Odin in 1976 by the IAU. A large volcanic dome 7 km in diameter and 1.4 km high is situated near the center of Odin.Katterfeld, G.N. ''Volcanism on Mercury''. Bulletin of Volcanology 47, 531–535 (1984)doi.org/10.1007/BF01961224/ref> Odin Planitia is located east of the Caloris basin. The southern portion is mapped on the Tolstoj quadrangle, and the northern portion is on the Shakespeare quadrangle The Shakespeare quadrangle is a region of Mercury running from 90 to 180° longitude and 20 to 70° latitude. It is also called Caduceata. The Borealis quadrangle is north of Shakespeare quadrangle. To the west is Raditladi quadrangle, and to t .... References Surface features of Mercury {{crater-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Alpes Formation
Montes Alpes is a mountain range in the northern part of the Moon's near side. It was named after the Alps in Europe; the name was confirmed by the International Astronomical Union in 1935. It lies between the selenographic coordinates latitudes 52.81°N and 42.04°N, and longitudes 5.6°W and 3.22°E. The range thus crosses the lunar prime meridian, and is partially illuminated and partially in shadow during first and last quarters. The center of the range is at 48.36°N, 0.58°W, and has a diameter of 334 km. Description This range forms the northeastern border of the Mare Imbrium lunar mare. To the west of the range is the level and nearly featureless mare, while on the eastern face is a more rugged continental area with a higher albedo. The range begins about one crater diameter northwest of the crater Cassini, at the Promontorium Agassiz, then stretches about 280 kilometres to the northwest and continues in intermittent fashion and the mountains proper end shy of on ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Nervo (crater)
Nervo is a crater on Mercury. It has a diameter of 63 kilometers. Its name was adopted by the International Astronomical Union in 1979. Nervo is named for the Mexican poet Amado Nervo, who lived from 1870 to 1919. Hollows are present on and near the central peak of Nervo. To the east of Nervo are linear ridges trending radially from the Caloris basin, believed to be ejecta from the Caloris impact event, similar to Imbrium sculpture on the Moon The Moon is Earth's only natural satellite. It is the fifth largest satellite in the Solar System and the largest and most massive relative to its parent planet, with a diameter about one-quarter that of Earth (comparable to the width of .... File:Mariner 10 image 0000193.png, Mariner 10 image with Nervo below center File:Nervo crater MESSENGER NAC mosaic.jpg, MESSENGER NAC Mosaic of central Nervo References Impact craters on Mercury {{Mercury-planet-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mare Orientale
Mare Orientale (Latin ''orientāle'', the "eastern sea") is a lunar mare. It is located on the western border of the near side and far side of the Moon, and is difficult to see from an Earthbound perspective. Images from spacecraft have revealed it to be one of the most striking large scale lunar features, resembling a target ring bullseye. Geology During the 1960s, rectified images of Mare Orientale by Gerard Kuiper at the Lunar and Planetary Laboratory gave rise to the notion of it being an impact crater. The structure, with the flat plain of the mare in the center, is about across and was formed by the impact of an asteroid-sized object, possibly in diameter and travelling at . Compared with most other lunar basins, Mare Orientale is less flooded by mare basalts, so that much of the basin structure is visible. The basalt in the central portion of the Orientale basin is probably less than in thickness which is much less than mare basins on the Earth-facing side of the Moon. ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Apennine Bench Formation
Montes Apenninus are a rugged mountain range on the northern part of the Moon's near side. They are named after the Apennine Mountains in Italy. With their formation dating back about 3.9 billion years, Montes Apenninus are fairly old. Description This range forms the southeastern border of the large Mare Imbrium lunar mare and the northwestern border of the Terra Nivium highland region. It begins just to the west of the prominent crater Eratosthenes, which abuts against the southern face of the range. To the west of these mountains is a narrow gap where Mare Imbrium in the north joins Mare Insularum to the south. Further to the west are the Montes Carpatus mountains. From Eratosthenes, the mountains form an arcing chain that gradually bends from east to northeast, ending at Promontorium Fresnel at about latitude 29.5° N. Here is another gap where the Mare Imbrium to the west joins the Mare Serenitatis to the east. At the north end of this gap lie the Montes Caucasus. This r ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Massif
In geology, a massif ( or ) is a section of a planet's crust that is demarcated by faults or flexures. In the movement of the crust, a massif tends to retain its internal structure while being displaced as a whole. The term also refers to a group of mountains formed by such a structure. In mountaineering and climbing literature, a massif is frequently used to denote the main mass of an individual mountain. The massif is a smaller structural unit of the crust than a tectonic plate, and is considered the fourth-largest driving force in geomorphology. The word is taken from French (in which the word also means "massive"), where it is used to refer a large mountain mass or compact group of connected mountains forming an independent portion of a range. One of the most notable European examples of a massif is the Massif Central of the Auvergne region of France. The Face on Mars is an example of an extraterrestrial massif. Massifs may also form underwater, as with the Atlanti ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Caloris Montes
The Caloris Montes (Latin for "Heat's Mountains") are a range of mountains on Mercury. They are a system of linear hills and valleys that extend more than 1000 km to the northeast from the mountainous rim of Caloris Basin in the Shakespeare quadrangle (H-3). The range consists of numerous rectilinear massif In geology, a massif ( or ) is a section of a planet's crust that is demarcated by faults or flexures. In the movement of the crust, a massif tends to retain its internal structure while being displaced as a whole. The term also refers to a ...s 1 to 3 km high and about 10 to 50 km long, mostly elongated radially from the center of the basin and separated by hackly-floored, radial troughs and gouge-like structures. The surfaces of the massifs are hackly. They are best developed along the inner edge of the basin where steep inward-facing scarps are common, grading outward into smaller massifs and blocks. The range marks the crest of most prominent ring structure ar ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Caloris Basin
Caloris Planitia is a plain within a large impact basin on Mercury, informally named Caloris, about in diameter. It is one of the largest impact basins in the Solar System. "Calor" is Latin for "heat" and the basin is so-named because the Sun is almost directly overhead every second time Mercury passes perihelion. The crater, discovered in 1974, is surrounded by the Caloris Montes, a ring of mountains approximately tall. Appearance Caloris was discovered on images taken by the '' Mariner 10'' probe in 1974. Its name was suggested by Brian O'Leary, astronaut and member of the ''Mariner 10'' imagery team. It was situated on the terminator—the line dividing the daytime and nighttime hemispheres—at the time the probe passed by, and so half of the crater could not be imaged. Later, on January 15, 2008, one of the first photos of the planet taken by the '' MESSENGER'' probe revealed the crater in its entirety. The basin was initially estimated to be about in diameter, thoug ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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