|
Outflow Channel
Outflow channels are extremely long, wide swathes of scoured ground on Mars. 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, 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 million years, extremely young by the standards of Martian topographic features. The largest, Kasei Vallis, is around long, greater than wide and exceeds in depth cut into the surrounding plains. The outflow channels contrast with the Martian channel features known as " valley networks", which much more closely resemble the dendritic planform more typical of terrestrial river drainage basins. Outflow channels tend to be named after the names for Mars in various ancient world ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Kasei Valles Topo
Kasei () is the Japanese word for Mars. It may refer to: Places * Kasei Valles, a canyon on Mars * Kasei, Kenya, a village in Kenya * Kasei, Ghana, a village in Ghana Transportation * Mitsubishi Kasei, a World War II aircraft engine used on many Japanese warplanes * Kasei Station, a train station on the Fujikyuko Line in Tsuru, Yamanashi, Japan * Toritsu-Kasei Station, a train station on the Seibu Shinjuku Line in Nakano, Tokyo, Japan Educational institutions * Tokyo Kasei-Gakuin University, a private university in Tokyo * Tokyo Kasei-Gakuin Junior College, a women's university in Tokyo * Tokyo Kasei University, a private university in Tokyo Other * Asahi Kasei is a multinational Japanese chemical company. Its main products are chemicals and materials science. It was founded in May 1931, using the paid in capital of Nobeoka Ammonia Fiber Co., Ltd, a Nobeoka, Miyazaki based producer of ammonia, nitri ..., a Japanese chemical conglomerate * Rakuto Kasei, a Japanese mul ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Igneous Activity
Volcanism, vulcanism or volcanicity is the phenomenon of eruption of molten rock (magma) onto the surface of the Earth or a solid-surface planet or moon, where lava, pyroclastics, and volcanic gases erupt through a break in the surface called a vent. It includes all phenomena resulting from and causing magma within the crust or mantle of the body, to rise through the crust and form volcanic rocks on the surface. Magmas, that reach the surface and solidify, form extrusive landforms. Volcanic processes Magma from the mantle or lower crust rises through the crust towards the surface. If magma reaches the surface, its behavior depends on the viscosity of the molten constituent rock. Viscous (thick) magma produces volcanoes characterised by explosive eruptions, while non-viscous (runny) magma produce volcanoes characterised by effusive eruptions pouring large amounts of lava onto the surface. In some cases, rising magma can cool and solidify without reaching the surface. Instead, ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Ganges Chasma
Ganges Chasma is a deep canyon at the eastern end of the vast Valles Marineris system on Mars, an offshoot of Capri Chasma, and is in the Coprates quadrangle. It is named after the River Ganges in South Asia. Ganges Chasma is thought to have formed through a series of catastrophic discharges of water and CO2 from chaos terrains such as that preserved in Ganges Chaos at its southern margin. Most of the evidence for these discharges and the ensuing collapses is believed to have been washed away. Prior to developing an outlet that joined it to Capri Chasma and the connected outflow channels to its east, Ganges Chasma may at some point in the Noachian period have contained a lake which drained northward through partially subsurface pathways into Shalbatana Vallis. File:Xantheterra6.jpg, Map of Xanthe Terra that shows location of Ganges Chasma and other major features Image:Ganges Chasma.JPG, Cliff in northern wall of Ganges Chasma, as seen by THEMIS. Click on image to see relatio ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Orson Welles (crater)
Orson Welles is an impact crater in the Coprates quadrangle of Mars, located at 0.2° S and 45.9° W. It is 124.5 kilometers in diameter and was named after Orson Welles (1915–1985), an American radio and motion picture actor and director. He is famous for, among other things, his radio broadcast of ''The War of the Worlds'' by H. G. Wells in which Martians invade Earth. The layers and the clay minerals found in Orson Welles Crater are evidence that it once contained a lake. File:Xantheterra6.jpg, Map of Xanthe Terra showing location of Orson Welles Crater and other major features Wikiorson.jpg, Western side of Orson Welles Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Dark areas on floor are dunes. Wikiorsondunes.jpg, Dunes on floor of Orson Welles Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Small curved channels are also visible. Note: this is an enlargement of previous photo. See also * Impact crater * Impact event * Lakes on Mars * L ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Shalbatana Vallis
Shalbatana Vallis is an ancient water-worn channel on Mars, located in the Oxia Palus quadrangle at 7.8° north latitude and 42.1° west longitude. It is the westernmost of the southern Chryse outflow channels. Beginning in a zone of chaotic terrain, at 0° latitude and 46° W longitude, it ends in Chryse Planitia. Shalbatana Vallis contains the first definitive evidence of a Martian shoreline. This shoreline was part of an ancient lake in size and deep. The study carried out with HiRISE images indicates that water formed a long canyon that opened up into a valley, deposited sediment, and created a delta. This delta and others around the basin imply the existence of a large, long-lived lake. Of special interest is evidence that the lake formed after the warm, wet period was thought to have ended. So, lakes may have been around much longer than previously thought. It is the word for "Mars" in Akkadian. File:Quadrângulo de Oxia Palus.JPG, Quadrangle map of Oxia Palus labele ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Ravi Vallis
Ravi Vallis is an ancient outflow channel, the source of which originates from the Aromatum Chaos depression, and is situated at the eastern end of Xanthe Terra, in the Margaritifer Sinus quadrangle (MC-19) region of Mars, located at . The Ravi Vallis outflow channel is long, and starts at the northeastern end of the Aromatum Chaos depression. The channel is orientated in an easterly direction, and further down channel, Ravi Vallis divides into two; a larger northern channel, and a smaller southern channel, and is finally truncated by a fault which is located at the western margin of the Hydraotes Chaos depression. Ravi Vallis was named after the Ravi River, an ancient Indian river. The Ravi Vallis outflow channel and neighboring deep depression at Aromatum Chaos, are thought to have been caused by volcano-ice interactions underneath the surface, which pierced an underground aquifer. This released large amounts of water, causing a catastrophic flood event, with an estimated speed ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mawrth Vallis
Mawrth Vallis () (Mawrth means "Mars" in Welsh) is a valley on Mars, located in the Oxia Palus quadrangle at 22.3°N, 343.5°E with an elevation approximately two kilometers below datum. Situated between the southern highlands and northern lowlands, the valley is a channel formed by massive flooding which occurred in Mars’ ancient past. It is an ancient water outflow channel with light-colored clay-rich rocks. Prior to the selection of Gale Crater for the Mars Science Laboratory (MSL) ''Curiosity'' rover mission, Mawrth Vallis was considered as a potential landing site because of the detection of a stratigraphic section rich in clay minerals. Clay minerals have implications for past aqueous environments as well as the potential to preserve biosignatures, making them ideal targets for the search for life on Mars. Although Mawrth Vallis was not chosen as a landing target, there is still interest in understanding the mineralogy and stratigraphy of the area. Until a rover mission ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Juventae Chasma
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. Juventae Chasma is located north of Valles Marineris in the Coprates quadrangle and cuts more than 5 km into the plains of Lunae Planum. Name Juventae was named by Giovanni Schiaparelli after the mythical ''Juventae Fons'', the fountain of youth. Observations The floor of Juventae Chasma is partly covered by sand dunes. There is also a 2.5 km high mountain inside Juventae, 59 km long and 23 km wide, that was confirmed by Mars Express to be composed of sulfate deposits. MRO discovered sulfates, hydrated sulfates, and iron oxides in Juventae Chasma. Juventae Chasma has four bright mounds or light-toned interior layered deposits (IlD's), as they are often called. Researchers have found that monohydrated sulfates were first deposited on the floor. And then polyhydrated sulfates were laid down. Kieserite, a magne ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Maja Valles
The Maja Valles are a large system of ancient outflow channels in the Lunae Palus quadrangle on Mars. 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 be have formed through water erosion.Keske, A., P. Christensen. 2017. MAJA VALLES: A MULTI-SOURCE FLUVIO-VOLCANIC OUTFLOW CHANNEL SYSTEM. Lunar and Planetary Science XLVIII (2017). 2985pdf. ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Echus Chasma
Echus Chasma is a chasma in the Lunae Planum high plateau north of the Valles Marineris canyon system of Mars. It is in the Coprates quadrangle.ESA (2008-07-14). Echus Chasma. Retrieved on 2008-07-15 from http://www.esa.int/esaSC/SEM4CATHKHF_index_0.html. Clay has been found within it, meaning that water once sat there for a time. It may have been one of the many lakes that have been advanced for the Martian past. Research from 2010 suggests that Mars had lakes along parts of the equator, which is where Echus Chasma lies. Although earlier research had showed that Mars had a warm and wet early history that has long since dried up, these lakes existed in the Hesperian Epoch, a much later period. Using detailed images from NASA's Mars Reconnaissance Orbiter, the researchers speculate that there may have been increased volcanic activity, meteorite impacts or shifts in Mars' orbit during this period to warm Mars' atmosphere enough to melt the abundant ice present in the ground. Volca ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Iani Chaos
Iani Chaos is a region of chaos terrain at the south end of the outflow channel Ares Vallis, of the Margaritifer Sinus quadrangle (MC-19) region of the planet Mars, centered at approximately ~342°E, 2°S. This is the source region of Ares Vallis. The chaotic terrain is widely believed to have formed via the removal of subsurface water or ice, resulting in flooding at the surface, and the formation of Ares Vallis. Within Iani Chaos, deposited stratigraphically above the chaotic terrain, are smooth, low-slope, intermediate-to-light-toned deposits that are rich in a hydrated mineral that is most likely gypsum as well as hematite. Mapbeer.jpg, Map showing location of Arsinoes Chaos (far left), Iani Chaos, Aureum Chaos, Margaritifer Chaos, and other nearby features Mars Science Laboratory Several sites in the Margaritifer Sinus quadrangle have been proposed as areas to send NASA's next major Mars rover, the Mars Science Lab. Among the top 33 landing sites was Iani Chaos. A picture ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Aram Chaos
Aram Chaos, centered at 2.6°N, 21.5°W, is a heavily eroded impact crater on Mars. It lies at the eastern end of the large canyon Valles Marineris and close to Ares Vallis. Various geological processes have reduced it to a circular area of chaotic terrain. Aram Chaos takes its name from Aram, one of the classical albedo features observed by Giovanni Schiaparelli, who named it after the Biblical land of Aram. Spectroscopic observation from orbit indicates the presence of the mineral hematite, likely a signature of a once aqueous environment. Description Aram Chaos is an impact crater on Mars measuring 280 kilometers (170 mi) in diameter. It lies in the Oxia Palus quadrangle in a region called Margaritifer Terra, and its exact coordinates on Mars are . The Thermal Emission Imaging System (THEMIS) on the orbiter ''Mars Odyssey'' found gray crystalline hematite on the floor of Aram Chaos and CRISM, the spectroscope on the MRO, found hydrated sulfates, jarosite, and hematite. The ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
