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Montes Agricola
Montes Agricola is an elongated range of mountains near the eastern edge of the central Oceanus Procellarum lunar mare. It lies just to the northwest of a plateau containing the craters Herodotus and Aristarchus. The selenographic coordinates of this range are . It continues for a distance of 160 kilometres. This range is a long, slender ridge formation that is more rugged at the northeastern end. There is also a rise at the southwest terminus of the range. The faint trace of a ray parallels the range just to the north. The 20 km gap between this range and the plateau to the south is covered by a flow of basaltic lava. There is a small wrinkle ridge near the northern part that is identified as Dorsum Niggli. This range is named after Georgius Agricola. External links LTO-38B2 Nielsen— L&PI topographic map In modern mapping, a topographic map or topographic sheet is a type of map characterized by large- scale detail and quantitative representation of relief fe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lunar Reconnaissance Orbiter
The Lunar Reconnaissance Orbiter (LRO) is a NASA robotic spacecraft currently orbiting the Moon in an eccentric polar mapping orbit. Data collected by LRO have been described as essential for planning NASA's future human and robotic missions to the Moon. Its detailed mapping program is identifying safe landing sites, locating potential resources on the Moon, characterizing the radiation environment, and demonstrating new technologies. Launched on June 18, 2009, in conjunction with the Lunar Crater Observation and Sensing Satellite (LCROSS), as the vanguard of NASA's Lunar Precursor Robotic Program, LRO was the first United States mission to the Moon in over ten years. LRO and LCROSS were launched as part of the United States's Vision for Space Exploration program. The probe has made a 3-D map of the Moon's surface at 100-meter resolution and 98.2% coverage (excluding polar areas in deep shadow), including 0.5-meter resolution images of Apollo landing sites. The first images f ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Mountains On The Moon
Mountains on the Moon have heights defined relative to various vertical datums. In the 1960s, the U.S. Army Mapping Service used elevation relative to 1,737,988 meters from the center of the Moon. In the 1970s, the U.S. Defense Mapping Agency used 1,730,000 meters. The '' Clementine'' topographic data published in the 1990s uses 1,737,400 meters. This table is not comprehensive, and does not list the highest places on the Moon. ''Clementine'' data show a range of about 18,100 meters from lowest to highest point on the Moon. The highest point, located on the far side of the Moon, is approximately 6,500 meters higher than Mons Huygens (usually listed as the tallest mountain). Mountains These are isolated mountains or massifs. Mountain ranges See also *List of mountains on the Moon by height *List of features on the Moon *List of craters on the Moon * List of maria on the Moon *List of valleys on the Moon *List of mountain ranges *List of tallest mountains in the Solar Syste ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 Australia). The Moon is a planetary-mass object with a differentiated rocky body, making it a satellite planet under the geophysical definitions of the term and larger than all known dwarf planets of the Solar System. It lacks any significant atmosphere, hydrosphere, or magnetic field. Its surface gravity is about one-sixth of Earth's at , with Jupiter's moon Io being the only satellite in the Solar System known to have a higher surface gravity and density. The Moon orbits Earth at an average distance of , or about 30 times Earth's diameter. Its gravitational influence is the main driver of Earth's tides and very slowly lengthens Earth's day. The Moon's orbit around Earth has a sidereal period of 27.3 days. During each synodic period ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Montes Agricola
Montes Agricola is an elongated range of mountains near the eastern edge of the central Oceanus Procellarum lunar mare. It lies just to the northwest of a plateau containing the craters Herodotus and Aristarchus. The selenographic coordinates of this range are . It continues for a distance of 160 kilometres. This range is a long, slender ridge formation that is more rugged at the northeastern end. There is also a rise at the southwest terminus of the range. The faint trace of a ray parallels the range just to the north. The 20 km gap between this range and the plateau to the south is covered by a flow of basaltic lava. There is a small wrinkle ridge near the northern part that is identified as Dorsum Niggli. This range is named after Georgius Agricola. External links LTO-38B2 Nielsen— L&PI topographic map In modern mapping, a topographic map or topographic sheet is a type of map characterized by large- scale detail and quantitative representation of relief fe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mountain
A mountain is an elevated portion of the Earth's crust, generally with steep sides that show significant exposed bedrock. Although definitions vary, a mountain may differ from a plateau in having a limited Summit (topography), summit area, and is usually higher than a hill, typically rising at least 300 metres (1,000 feet) above the surrounding land. A few mountains are Monadnock, isolated summits, but most occur in mountain ranges. Mountain formation, Mountains are formed through Tectonic plate, tectonic forces, erosion, or volcanism, which act on time scales of up to tens of millions of years. Once mountain building ceases, mountains are slowly leveled through the action of weathering, through Slump (geology), slumping and other forms of mass wasting, as well as through erosion by rivers and glaciers. High elevations on mountains produce Alpine climate, colder climates than at sea level at similar latitude. These colder climates strongly affect the Montane ecosystems, ecosys ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Oceanus Procellarum
Oceanus Procellarum ( la, Ōceanus procellārum, lit=Ocean of Storms) is a vast lunar mare on the western edge of the near side of the Moon. It is the only one of the lunar maria to be called an "Oceanus" (ocean), due to its size: Oceanus Procellarum is the largest of the maria ("seas"), stretching more than across its north–south axis and covering roughly , accounting for 10.5% of the total lunar surface area. Characteristics Like all lunar maria, Oceanus Procellarum was formed by ancient volcanic eruptions resulting in basaltic floods that covered the region in a thick, nearly flat layer of solidified magma. Basalts in Oceanus Procellarum have been estimated to be as young as one billion years old. Unlike the other lunar maria, however, Oceanus Procellarum may or may not be contained within a single, well-defined impact basin. Around its edges lie many minor bays and seas, including Sinus Roris to the north, and Mare Nubium and Mare Humorum to the south. To the northeast, ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lunar Mare
The lunar maria (; singular: mare ) are large, dark, basaltic plains on Earth's Moon, formed by ancient asteroid impacts on the far side on the Moon that triggered volcanic activity on the opposite (near) side. They were dubbed , Latin for 'seas', by early astronomers who mistook them for actual seas. They are less reflective than the "highlands" as a result of their iron-rich composition, and hence appear dark to the naked eye. The maria cover about 16% of the lunar surface, mostly on the side visible from Earth. The few maria on the far side are much smaller, residing mostly in very large craters. The traditional nomenclature for the Moon also includes one (ocean), as well as features with the names ('lake'), ('marsh'), and ('bay'). The last three are smaller than maria, but have the same nature and characteristics. The names of maria refer to sea features (Mare Humorum, Mare Imbrium, Mare Insularum, Mare Nubium, Mare Spumans, Mare Undarum, Mare Vaporum, Oceanus Procellarum ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Herodotus (crater)
Herodotus is a lunar impact crater located on a low shelf in the midst of the Oceanus Procellarum. To the east is the slightly larger crater Aristarchus. West across the mare is Schiaparelli. Almost due south on the mare surface is a solitary lunar dome designated Herodotus Omega (ω). The crater Herodotus has a slightly irregular, narrow rim that appears somewhat oblong due to foreshortening. The inner floor has been flooded with lava, and has a lower albedo than its brighter and more prominent neighbor Aristarchus. There is a small craterlet overlapping the northwest rim, but otherwise the outer wall has not suffered significant wear. Nevertheless, the rim is unusually thin in relation to its size. To the north of Herodotus is the start of the Vallis Schröteri, a valley that has a length of 160 kilometers and a maximum depth of nearly a kilometer. It begins at a small crater 25 km north of the rim, then winds across the surface to the north, before turning northwest ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Aristarchus (crater)
Aristarchus is a lunar impact crater that lies in the northwest part of the Moon's near side. It is considered the brightest of the large formations on the lunar surface, with an albedo nearly double that of most lunar features. The feature is bright enough to be visible to the naked eye, and displays unusually bright features when viewed through a large telescope. It is also readily identified when most of the lunar surface is illuminated by earthshine. The crater is deeper than the Grand Canyon. The crater is named after the Greek astronomer Aristarchus of Samos. It is located at the southeastern edge of the Aristarchus plateau, an elevated area that contains a number of volcanic features, such as sinuous rilles. This area is also noted for the large number of reported transient lunar phenomena, as well as recent emissions of radon gas as measured by the Lunar Prospector spacecraft. Selenography Aristarchus is located on the Aristarchus plateau, an elevated rocky rise ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Selenographic Coordinates
The selenographic coordinate system is used to refer to locations on the surface of Earth's moon. Any position on the lunar surface can be referenced by specifying two numerical values, which are comparable to the latitude and longitude of Earth. The longitude gives the position east or west of the Moon's prime meridian, which is the line passing from the lunar north pole through the point on the lunar surface directly facing Earth to the lunar south pole. (See also Earth's prime meridian.) This can be thought of as the midpoint of the visible Moon as seen from the Earth. The latitude gives the position north or south of the lunar equator. Both of these coordinates are given in degrees. Astronomers defined the fundamental location in the selenographic coordinate system by the small, bowl-shaped satellite crater ' Mösting A'. The coordinates of this crater are defined as: : Later, the coordinate system has become more precisely defined due to the Lunar Laser Ranging E ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Ray System
A ray system comprises radial streaks of fine '' ejecta'' thrown out during the formation of an impact crater, looking somewhat like many thin spokes coming from the hub of a wheel. The rays may extend for lengths up to several times the diameter of their originating crater, and are often accompanied by small secondary craters formed by larger chunks of ejecta. Ray systems have been identified on the Moon, Earth ( Kamil Crater), Mercury, and some moons of the outer planets. Originally it was thought that they existed only on planets or moons lacking an atmosphere, but more recently they have been identified on Mars in infrared images taken from orbit by '' 2001 Mars Odyssey''s thermal imager. Rays appear at visible, and in some cases infrared wavelengths, when ejecta are made of material with different reflectivity (i.e., albedo) or thermal properties from the surface on which they are deposited. Typically, visible rays have a higher albedo than the surrounding surface. More rarel ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Basalt
Basalt (; ) is an aphanite, aphanitic (fine-grained) extrusive igneous rock formed from the rapid cooling of low-viscosity lava rich in magnesium and iron (mafic lava) exposed at or very near the planetary surface, surface of a terrestrial planet, rocky planet or natural satellite, moon. More than 90% of all volcanic rock on Earth is basalt. Rapid-cooling, fine-grained basalt is chemically equivalent to slow-cooling, coarse-grained gabbro. The eruption of basalt lava is observed by geologists at about 20 volcanoes per year. Basalt is also an important rock type on other planetary bodies in the Solar System. For example, the bulk of the plains of volcanism on Venus, Venus, which cover ~80% of the surface, are basaltic; the lunar mare, lunar maria are plains of flood-basaltic lava flows; and basalt is a common rock on the surface of Mars. Molten basalt lava has a low viscosity due to its relatively low silica content (between 45% and 52%), resulting in rapidly moving lava flo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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