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Chryse Planitia
Chryse Planitia (Greek, "''Golden Plain''") is a smooth circular plain in the northern equatorial region of Mars close to the Tharsis region to the west, centered at . Chryse Planitia lies partially in the Lunae Palus quadrangle, partially in the Oxia Palus quadrangle, partially in the Mare Acidalium quadrangle. It is 1600 km or 994 mi in diameter and with a floor 2.5 km below the average planetary surface altitude, and has been suggested to be an ancient buried impact basin, though this is contested. It has several features in common with lunar maria, such as wrinkle ridges. The density of impact craters in the range is close to half the average for lunar maria. Chryse Planitia shows evidence of water erosion in the past, and is the bottom end for many outflow channels from the southern highlands as well as from Valles Marineris and the flanks of the Tharsis bulge. It is one of the lowest regions on Mars ( below the mean surface elevation of Mars), so water w ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Mars Viking 11h016
Mars is the fourth planet from the Sun. It is also known as the "Red Planet", because of Mars surface color, its orange-red appearance. Mars is a desert-like rocky planet with a tenuous carbon dioxide () Atmosphere of Mars, atmosphere. At the average surface level the atmospheric pressure is a few thousandths of Earth's, atmospheric temperature ranges from and cosmic radiation is high. Mars retains some water, Groundwater on Mars, in the ground as well as thinly in the atmosphere, forming cirrus clouds, frost, larger polar regions of permafrost and Martian polar ice caps, ice caps (with seasonal snow), but no liquid surface water. Its surface gravity is roughly a third of Earth's or double that of the Moon. It is half List of Solar System objects by size, as wide as Earth or twice the Moon, with a diameter of , and has a surface area the size of all the dry land of Earth. Martian regolith#Atmospheric dust, Fine dust is prevalent across the surface and the atmosphere, bein ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Maja Valles
The Maja Valles are a large system of ancient outflow channels in the Lunae Palus quadrangle on Mars. About Their location is 12.6° north latitude and 58.3° west longitude. The name is a Nepali word for "Mars". The Maja Valles begin at Juventae Chasma. Parts of the system have been partially buried by thin volcanic debris. The channels end at Chryse Planitia. Huge outflow channels were found in many areas by the Viking Orbiters. They showed that floods of water broke through dams, carved deep valleys, eroded grooves into bedrock, and traveled thousands of kilometers. The Maja Valles show evidence of lava flows in the northern section. Studies with HiRISE and CTX images suggest that the lava flows did not reach the turbulence necessary to erode large channels. So, the Maja Valles are believed to have been formed through water erosion.Keske, A., P. Christensen. 2017. MAJA VALLES: A MULTI-SOURCE FLUVIO-VOLCANIC OUTFLOW CHANNEL SYSTEM. Lunar and Planetary Science XLVIII (2 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Fluvial
A river is a natural stream of fresh water that flows on land or inside caves towards another body of water at a lower elevation, such as an ocean, lake, or another river. A river may run dry before reaching the end of its course if it runs out of water, or only flow during certain seasons. Rivers are regulated by the water cycle, the processes by which water moves around the Earth. Water first enters rivers through precipitation, whether from rainfall, the runoff of water down a slope, the melting of glaciers or snow, or seepage from aquifers beneath the surface of the Earth. Rivers flow in channeled watercourses and merge in confluences to form drainage basins, or catchments, areas where surface water eventually flows to a common outlet. Rivers have a great effect on the landscape around them. They may regularly overflow their banks and flood the surrounding area, spreading nutrients to the surrounding area. Sediment or alluvium carried by rivers shapes the landscape a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
North Polar Basin (Mars)
The North Polar Basin, more commonly known as the Borealis Basin, is a large basin in the northern hemisphere of Mars that covers 40% of the planet. Some scientists have postulated that the basin formed during the impact of a single, large body roughly 2% of the mass of Mars, having a diameter of about 1,900 km (1,200 miles) early in the history of Mars, around 4.5 billion years ago. However, the basin is not currently recognized as an impact basin by the IAU. The basin is one of the flattest areas in the Solar System, and has an elliptical shape. Large regions within the Borealis Basin Because the Borealis basin covers 40% of the surface of Mars, and much of the Northern Hemisphere, many currently recognized regions of Mars lie within it: * Acidalia Planitia * Arcadia Planitia * Planum Boreum * Utopia Planitia * Vastitas Borealis Borealis Impact Formation of the Borealis Basin One possible explanation for the basin's low, flat and relatively crater-free to ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Outflow Channels
Outflow channels are extremely long, wide swathes of scoured ground on Mars.Carr, M.H. (2006), ''The Surface of Mars''. Cambridge Planetary Science Series, Cambridge University Press. They extend many hundreds of kilometers in length and are typically greater than one kilometer in width. They are thought to have been carved by huge outburst floods. Crater counts indicate that most of the channels were cut since the early Hesperian,Hartmann, W.K., and Neukum, G. (2001). "Cratering chronology and the evolution of Mars". In: ''Chronology and Evolution of Mars'', ed. R. Kallenbach et al. Dordrecht: Kluwer, p. 165-94. though the age of the features is variable between different regions of Mars. Some outflow channels in the Amazonis and Elysium Planitiae regions have yielded ages of only tens of millions of years, extremely young by the standards of Martian topographic features.Burr, D.M., McEwan, A.S., and Sakimoto, S.E. (2002). "Recent aqueous floods from the Cerberus Fossae", ''M ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Amazonian Age
The geological history of Mars follows the physical evolution of Mars as substantiated by observations, indirect and direct measurements, and various inference techniques. Methods dating back to 17th-century techniques developed by Nicholas Steno, including the so-called law of superposition and stratigraphy, used to estimate the geological histories of Earth and the Moon, are being actively applied to the data available from several Martian observational and measurement resources. These include landers, orbiting platforms, Earth-based observations, and Martian meteorites. Observations of the surfaces of many Solar System bodies reveal important clues about their evolution. For example, a lava flow that spreads out and fills a large impact crater is likely to be younger than the crater. On the other hand, a small crater on top of the same lava flow is likely to be younger than both the lava and the larger crater since it can be surmised to have been the product of a later, unobs ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Hesperian
The Hesperian is a system (stratigraphy), geologic system and geologic timescale, time period on the planet Mars characterized by widespread Volcanology of Mars, volcanic activity and catastrophic flooding that carved immense outflow channels across the surface. The Hesperian is an intermediate and transitional period of Martian history. During the Hesperian, Mars changed from the wetter and perhaps warmer world of the Noachian (Mars), Noachian to the dry, cold, and dusty planet seen today. The absolute age of the Hesperian Period is uncertain. The beginning of the period followed the end of the Late Heavy Bombardment and probably corresponds to the start of the lunar Late Imbrian period, around 3700 million years ago (Myr, Mya). The end of the Hesperian Period is much more uncertain and could range anywhere from 3200 to 2000 Mya, with 3000 Mya being frequently cited. The Hesperian Period is roughly coincident with the Earth's early Archean Eon. With the decline of heavy impacts a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Bahram Vallis
Bahram Vallis is an ancient river valley in the Lunae Palus quadrangle of Mars at 20.7° north latitude and 57.5° west longitude. It is about 302 km long and was named after the word for 'Mars' in Persian. Bahram Vallis is located midway between Vedra Valles and lower Kasei Valles. It is basically a single trunk valley, with scalloped walls in some places. The presence of streamlined erosional features on its floor shows that fluid was involved with its formation.Baker, V. 1982. The Channels of Mars. University of Texas Press. Austin Image:Kasei Valles topolabled.JPG, Area around Northern Kasei Valles, showing relationships among Kasei Valles, Bahram Vallis, Vedra Valles, Maumee Valles, and Maja Valles. Map location is in Lunae Palus quadrangle and includes parts of Lunae Planum and Chryse Planitia. Image:Bahram Vallis.JPG, Bahram Vallis, as seen by HiRISE. Rotational landslides (slumps) are visible at the base of north wall. File:ESP 056904 2015valley.jpg, Close ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Maumee Valles
The Maumee Valles are a set of channels in an ancient river valley in the Lunae Palus quadrangle of Mars, located at 19.7° N and 53.2° W. They are long and were named after a North American river in Indiana and Ohio. Together with other ancient river valleys, they have provided strong evidence for a great deal of running water on the surface of Mars.Moore, P. et al. 1990. The Atlas of the Solar System. Mitchell Beazley Publishers NY, NY. Image:Kasei Valles topolabled.JPG, Area around the Northern Kasei Valles, showing relationships among Bahram Vallis and the Kasei Valles, Vedra Valles, Maumee Valles, and Maja Valles. Map location is in Lunae Palus quadrangle and includes parts of Lunae Planum and Chryse Planitia. Vallesmaumeevedrabox.jpg, Map showing relative positions of several channel systems in Lunae Palus quadrangle, including the Vedra Valles, Maumee Valles, and Maja Valles. Box indicates where these valleys can be found. Colors show elevation. See also * G ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Vedra Valles
The Vedra Valles are a set of channels in an ancient river valley in the Lunae Palus quadrangle of Mars, located at 19.4° N and 55.6° W. They are 115 km long and were named after an ancient river in Great Britain. Together with other ancient river valleys, they have provided strong evidence for a great deal of running water on the surface of Mars.Moore, P. et al. 1990. The Atlas of the Solar System. Mitchell Beazley Publishers NY, NY. Image:Kasei Valles topolabled.JPG, Area around the Northern Kasei Valles, showing relationships among Bahram Vallis and the Kasei Valles, Vedra Valles, Maumee Valles, and Maja Valles. Map location is in Lunae Palus quadrangle and includes parts of Lunae Planum and Chryse Planitia. Vallesmaumeevedrabox.jpg, Map showing relative positions of several channel systems in the Lunae Palus quadrangle, including the Vedra Valles, Maumee Valles, and Maja Valles. Box indicates their location; colors designate elevation. See also * Geology of Ma ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Viking Program
The ''Viking'' program consisted of a pair of identical American space probes, ''Viking 1'' and ''Viking 2'' both launched in 1975, and landed on Mars in 1976. The mission effort began in 1968 and was managed by the NASA Langley Research Center.Soffen, G. A. (July–August 1978). "Mars and the Remarkable Viking Results." ''Journal of Spacecraft and Rockets''. 15 (4): 193-200. Each spacecraft was composed of two main parts: an orbiter spacecraft which photographed the surface of Mars from orbit, and a Lander (spacecraft), lander which studied the planet from the surface. The orbiters also served as communication relays for the landers once they touched down. The Viking program grew from NASA's earlier, even more ambitious, Voyager program (Mars), Voyager Mars program, which was not related to the successful Voyager program, Voyager deep space probes of the late 1970s. ''Viking 1'' was launched on August 20, 1975, and the second craft, ''Viking 2'', was launched on September 9, ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
Simud Valles
The Simud Valles are an ancient outflow channel system in the Oxia Palus quadrangle of Mars, located at 19.8° N and 37.8° W. They are 945 km long and were named for the word for "Mars" in Sumerian. Note: Descriptor term changed to the plural (valles), and coordinates redefined 3/31/2008. See also * Geology of Mars * HiRISE * Outflow channels Outflow channels are extremely long, wide swathes of scoured ground on Mars.Carr, M.H. (2006), ''The Surface of Mars''. Cambridge Planetary Science Series, Cambridge University Press. They extend many hundreds of kilometers in length and are typi ... References Further reading * * Valleys and canyons on Mars Oxia Palus quadrangle {{mars-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] [Amazon] |
