|
Mamers Valles
The Mamers Valles are a set of channels in a long, winding canyon in the north of Mars. They cover 1000 km, cutting through the cratered uplands of the Arabia Terra, from the Cerulli crater to the Deuteronilus Mensae near the edge of Mars' vast northern lowlands. Through their midsection, they average a width of 25 km and a depth of 1200 meters. Theories of canyon formation include that Mamers Valles were formed by either water or lava, with the flow from south to north and additional material flowing from the slope toward the valley floor. According to the most popular theory, linear features on the valley bottom indicate possible ice flows and that ice may currently be plentiful. The Mamers Valles are dated to the early Hesperian period, about 3.8 billion years ago. An infeeder canyon at the northwestern edge of the Mamers Valles, near their mouth (seen at the bottom of the photo at lower right), is a box canyon. Such canyons (with rounded headwalls and no obvious ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mamers Valles
The Mamers Valles are a set of channels in a long, winding canyon in the north of Mars. They cover 1000 km, cutting through the cratered uplands of the Arabia Terra, from the Cerulli crater to the Deuteronilus Mensae near the edge of Mars' vast northern lowlands. Through their midsection, they average a width of 25 km and a depth of 1200 meters. Theories of canyon formation include that Mamers Valles were formed by either water or lava, with the flow from south to north and additional material flowing from the slope toward the valley floor. According to the most popular theory, linear features on the valley bottom indicate possible ice flows and that ice may currently be plentiful. The Mamers Valles are dated to the early Hesperian period, about 3.8 billion years ago. An infeeder canyon at the northwestern edge of the Mamers Valles, near their mouth (seen at the bottom of the photo at lower right), is a box canyon. Such canyons (with rounded headwalls and no obvious ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Oscan
Oscan is an extinct Indo-European language of southern Italy. The language is in the Osco-Umbrian or Sabellic branch of the Italic languages. Oscan is therefore a close relative of Umbrian. Oscan was spoken by a number of tribes, including the Samnites, the Aurunci ( Ausones), and the Sidicini. The latter two tribes were often grouped under the name "Osci". The Oscan group is part of the Osco-Umbrian or Sabellic family, and includes the Oscan language and three variants ( Hernican, Marrucinian and Paelignian) known only from inscriptions left by the Hernici, Marrucini and Paeligni, minor tribes of eastern central Italy. Adapted from the Etruscan alphabet, the Central Oscan alphabet was used to write Oscan in Campania and surrounding territories from the 5th century BCE until possibly the 1st century CE. Evidence Oscan is known from inscriptions dating as far back as the 5th century BCE. The most important Oscan inscriptions are the Tabula Banti ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Glacial Landscape Near Mamers Valles
A glacial period (alternatively glacial or glaciation) is an interval of time (thousands of years) within an ice age that is marked by colder temperatures and glacier advances. Interglacials, on the other hand, are periods of warmer climate between glacial periods. The Last Glacial Period ended about 15,000 years ago. The Holocene is the current interglacial. A time with no glaciers on Earth is considered a greenhouse climate state. Quaternary Period Within the Quaternary, which started about 2.6 million years before present, there have been a number of glacials and interglacials. At least eight glacial cycles have occurred in the last 740,000 years alone. Penultimate Glacial Period The Penultimate Glacial Period (PGP) is the glacial period that occurred before the Last Glacial Period. It began about 194,000 years ago and ended 135,000 years ago, with the beginning of the Eemian interglacial. Last Glacial Period The last glacial period was the most recent glacial period wi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mars
Mars is the fourth planet from the Sun and the second-smallest planet in the Solar System, only being larger than Mercury (planet), Mercury. In the English language, Mars is named for the Mars (mythology), Roman god of war. Mars is a terrestrial planet with a thin atmosphere (less than 1% that of Earth's), and has a crust primarily composed of elements similar to Earth's crust, as well as a core made of iron and nickel. Mars has surface features such as impact craters, valleys, dunes and polar ice caps. It has two small and irregularly shaped moons, Phobos (moon), Phobos and Deimos (moon), Deimos. Some of the most notable surface features on Mars include Olympus Mons, the largest volcano and List of tallest mountains in the Solar System, highest known mountain in the Solar System and Valles Marineris, one of the largest canyons in the Solar System. The North Polar Basin (Mars), Borealis basin in the Northern Hemisphere covers approximately 40% of the planet and may be a la ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
USGS Astrogeology Science Center
The Astrogeology Science Center is the entity within the United States Geological Survey concerned with the study of planetary geology and planetary cartography. It is housed in the Shoemaker Building in Flagstaff, Arizona. The Center was established in 1963 by Eugene Merle Shoemaker to provide lunar geologic mapping and to assist in training astronauts destined for the Moon as part of the Apollo program. Since its inception, the Astrogeology Science Center has participated in processing and analyzing data from various missions to the planetary bodies in the Solar System, assisting in finding potential landing sites for exploration vehicles, mapping our neighboring planets and their moons, and conducting research to better understand the origins, evolutions, and geologic processes operating on these bodies. The Early Days Gene Shoemaker founded the Astrogeology Research Program August 25, 1960. The research program started out as the ''Astrogeologic Studies Group'' at the Uni ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Arabia Terra
Arabia Terra is a large upland region in the north of Mars that lies mostly in the Arabia quadrangle, but a small part is in the Mare Acidalium quadrangle. It is densely cratered and heavily eroded. This battered topography indicates great age, and Arabia Terra is presumed to be one of the oldest terrains on the planet. It covers as much as at its longest extent, centered roughly at with its eastern and southern regions rising above the north-west. Alongside its many craters, canyons wind through the Arabia Terra, many emptying into the large northern lowlands of the planet, which borders Arabia Terra to the north. Features Arabia contains many interesting features. There are some good examples of pedestal craters in the area. A pedestal crater has its ejecta above the surrounding terrain, often forming a steep cliff. The ejecta forms a resistant layer that protects the underlying material from erosion. Mounds and buttes on the floor of some craters display many layers. ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Cerulli (crater)
Cerulli is a crater in the Ismenius Lacus quadrangle on Mars with a diameter of 130 km. It lies in the northern hemisphere south of the very large crater Lyot. It is named after Vincenzo Cerulli, an Italian astronomer (1859–1927). Impact craters generally have a rim with ejecta around them; in contrast, volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak. The peak is caused by a rebound of the crater floor following the impact. If one measures the diameter of a crater, the original depth can be estimated with various ratios. Because of this relationship, researchers have found that many Martian craters contain a great deal of material; much of it is believed to be ice deposited when the climate was different. Sometimes, craters expose layers that were buried. Cerulli shows evidence of glacial activity in the past. The density of impact craters is used to determine the su ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Deuteronilus Mensae
Deuteronilus Mensae is a region on Mars 937 km across and centered at . It covers 344°–325° West and 40°–48° North. Deuteronilus region lies just to the north of Arabia Terra and is included in the Ismenius Lacus quadrangle. It is along the dichotomy boundary, that is between the old, heavily cratered southern highlands and the low plains of the northern hemisphere. The region contains flat-topped knobby terrain that may have been formed by glaciers at some time in the past. Deuteronilus Mensae is to the immediate west of Protonilus Mensae and Ismeniae Fossae. Glaciers persist in the region in modern times, with at least one glacier estimated to have formed as recently as 100,000 to 10,000 years ago. Recent evidence from the radar on the Mars Reconnaissance Orbiter has shown that parts of Deuteronilus Mensae do indeed contain ice. Source of ice It is now widely believed that ice accumulated in many areas of Mars, including Deuteronilus Mensae, when the planet's orbi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Northern Lowlands Of Mars
(Latin 'northern waste') is the largest lowland region of Mars. It is in the northerly latitudes of the planet and encircles the northern polar region. Vastitas Borealis is often simply referred to as the northern plains, northern lowlands or the North polar erg of Mars. The plains lie 4–5 km below the mean radius of the planet, and is centered at . A small part of Vastitas Borealis lies in the Ismenius Lacus quadrangle. The region was named by Eugene Antoniadi, who noted the distinct albedo feature of the Northern plains in his book ''La Planète Mars'' (1930). The name was officially adopted by the International Astronomical Union in 1973. Although it is not an officially recognized feature, the North Polar Basin makes up most of the lowlands in the Northern Hemisphere of Mars. As a result, Vastitas Borealis lies within the North Polar Basin, while Utopia Planitia, another very large basin, is adjacent to it. Some scientists have speculated the plains were covered ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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] |
Valleys And Canyons On Mars
A valley is an elongated low area often running between hills or mountains, which will typically contain a river or stream running from one end to the other. Most valleys are formed by erosion of the land surface by rivers or streams over a very long period. Some valleys are formed through erosion by glacial ice. These glaciers may remain present in valleys in high mountains or polar areas. At lower latitudes and altitudes, these glacially formed valleys may have been created or enlarged during ice ages but now are ice-free and occupied by streams or rivers. In desert areas, valleys may be entirely dry or carry a watercourse only rarely. In areas of limestone bedrock, dry valleys may also result from drainage now taking place underground rather than at the surface. Rift valleys arise principally from earth movements, rather than erosion. Many different types of valleys are described by geographers, using terms that may be global in use or else applied only locally. For ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
.svg "Click for more on -> Mars")
