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Antoniadi (Martian Crater)
Antoniadi is a crater on Syrtis Major Planum in the Syrtis Major quadrangle, Mars, located at 21.5° north latitude and 299.2° west longitude. It is long and was named after Eugène Michael Antoniadi, a Greek astronomer (1870-1944) who spent most of his life in France. There is evidence that Antoniadi Crater once contained rivers and lakes. The picture below shows an inverted channel in Antoniadi, as seen by HiRISE. Inverted channels formed from accumulated sediments that were cemented by minerals. These channels eroded into the surface, then the whole area was covered over with sediments. When the sediments were later eroded away, the place where the river channel existed remained because the hardened material were resistant to erosion. Inverted relief Some places on Mars show inverted relief. In these locations, a stream bed may be a raised feature, instead of a valley. The inverted former stream channels may be caused by the deposition of large rocks or due to cementat ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Syrtis Major Planum
Syrtis Major Planum is a "dark spot" (an albedo feature) located in the boundary between the northern lowlands and southern highlands of Mars just west of the impact basin Isidis in the Syrtis Major quadrangle. It was discovered, on the basis of data from Mars Global Surveyor, to be a low-relief shield volcano, but was formerly believed to be a plain, and was then known as Syrtis Major Planitia. The dark color comes from the basaltic volcanic rock of the region and the relative lack of dust. A selected landing site for the Mars 2020 rover mission is Jezero crater (at ) within the region. The northeastern region of Syrtis Major Planum was also considered a potential landing site. Geography and geology Syrtis Major is centered near at , extends some north from the planet's equator, and spans from west to east. It is in the Syrtis Major quadrangle. It encompasses a large slope from its western edge at Aeria dropping to its eastern edge at Isidis Planitia. It includes a ... [...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] |
Eugène Michel Antoniadi
Eugène Michel Antoniadi (Greek: ΕυγÎνιος Αντωνιάδης; 1 March 1870 – 10 February 1944) was a Greek-French astronomer. Biography Antoniadi was born in Istanbul (Constantinople) but spent most of his adult life in France, after being invited there by Camille Flammarion. He became a Fellow of the Royal Astronomical Society on 10 February 1899, and in 1890 he became one of the founding members of the British Astronomical Association (BAA). In 1892, he joined the BAA's Mars Section and became that section's Director in 1896. He became a member of the Société astronomique de France (SAF) in 1891. Flammarion hired Antoniadi to work as an assistant astronomer in his private observatory in Juvisy-sur-Orge in 1893. Antoniadi worked there for nine years. In 1902, he resigned from both the Juvisy observatory and from SAF. Antoniadi rejoined SAF in 1909. That same year, Henri Deslandres, Director of the Meudon Observeratory, provided him with access to the ' ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Syrtis Major Quadrangle
The Syrtis Major quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Syrtis Major quadrangle is also referred to as MC-13 (Mars Chart-13). The quadrangle covers longitudes 270° to 315° west and latitudes 0° to 30° north on Mars. Syrtis Major quadrangle includes Syrtis Major Planum and parts of Terra Sabaea and Isidis Planitia. Syrtis Major is an old shield volcano with a central depression that is elongated in a north–south direction. It contains the calderas Meroe Patera and Nili Patera. Interesting features in the area include dikes and inverted terrain. The ''Beagle 2'' lander was about to land near the quadrangle, particularly in the eastern part of Isidis Planitia, in December 2003, when contact with the craft was lost. In January 2015, NASA reported the ''Beagle 2'' had been found on the surface in Isidis Planitia (location is about ). High-resolution images captured b ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eugène Michael Antoniadi
Eugène Michel Antoniadi (Greek: ΕυγÎνιος Αντωνιάδης; 1 March 1870 – 10 February 1944) was a Greek- French astronomer. Biography Antoniadi was born in Istanbul (Constantinople) but spent most of his adult life in France, after being invited there by Camille Flammarion. He became a Fellow of the Royal Astronomical Society on 10 February 1899, and in 1890 he became one of the founding members of the British Astronomical Association (BAA). In 1892, he joined the BAA's Mars Section and became that section's Director in 1896. He became a member of the Société astronomique de France (SAF) in 1891. Flammarion hired Antoniadi to work as an assistant astronomer in his private observatory in Juvisy-sur-Orge in 1893. Antoniadi worked there for nine years. In 1902, he resigned from both the Juvisy observatory and from SAF. Antoniadi rejoined SAF in 1909. That same year, Henri Deslandres, Director of the Meudon Observeratory, provided him with access to the ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Inverted Relief
Inverted relief, inverted topography, or topographic inversion refers to landscape features that have reversed their elevation relative to other features. It most often occurs when low areas of a landscape become filled with lava or sediment that hardens into material that is more resistant to erosion than the material that surrounds it. ''Differential erosion'' then removes the less resistant surrounding material, leaving behind the younger resistant material, which may then appear as a ridge where previously there was a valley. Terms such as "inverted valley" or "inverted channel" are used to describe such features.Pain, C.F., and C.D. Ollier, 1995, ''Inversion of relief - a component of landscape evolution.'' Geomorphology. 12(2):151-165. Inverted relief has been observed on the surfaces of other planets as well as on Earth. For example, well-documented inverted topographies have been discovered on Mars.Pain, C.F., J.D.A. Clarke, and M. Thomas, 2007, ''Inversion of relief on ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Cementation (geology)
Cementation involves ions carried in groundwater chemically precipitating to form new crystalline material between sedimentary grains. The new pore-filling minerals forms "bridges" between original sediment grains, thereby binding them together. In this way, ''sand'' becomes sandstone, and ''gravel'' becomes conglomerate or breccia. Cementation occurs as part of the diagenesis or lithification of sediments. Cementation occurs primarily below the water table regardless of sedimentary grain sizes present. Large volumes of pore water must pass through sediment pores for new mineral cements to crystallize and so millions of years are generally required to complete the cementation process. Common mineral cements include calcite, quartz, and silica phases like cristobalite, iron oxides, and clay minerals; other mineral cements also occur. Cementation is continuous in the groundwater zone, so much so that the term "zone of cementation" is sometimes used interchangeably. Cementati ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Miyamoto (crater)
Miyamoto is a crater within the Margaritifer Sinus quadrangle (MC-19) region of the planet Mars, west of the Plains of Meridiani. It is wide. Its northeastern half is filled with rocks formed in the presence of water and include minerals of iron and sulfur, which likely settled on lake bottoms or in groundwater systems. In the southwestern half of the crater floor, erosion has stripped these materials away, revealing clays and other materials like those found in the most ancient Martian rocks. More than 3.5 billion years old, they date to the Noachian era at which time, liquid water was likely present at the surface and could have created an environment favorable to life. Miyamoto was considered as a possible landing site for the Mars Science Laboratory. 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 Laboratory. Miyamoto Crater was in the top seven sites chosen. ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Impact Crater
An impact crater is a circular depression in the surface of a solid astronomical object formed by the hypervelocity impact of a smaller object. In contrast to volcanic craters, which result from explosion or internal collapse, impact craters typically have raised rims and floors that are lower in elevation than the surrounding terrain. Lunar impact craters range from microscopic craters on lunar rocks returned by the Apollo Program and small, simple, bowl-shaped depressions in the lunar regolith to large, complex, multi-ringed impact basins. Meteor Crater is a well-known example of a small impact crater on Earth. Impact craters are the dominant geographic features on many solid Solar System objects including the Moon, Mercury, Callisto, Ganymede and most small moons and asteroids. On other planets and moons that experience more active surface geological processes, such as Earth, Venus, Europa, Io and Titan, visible impact craters are less common because they become eroded ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Impact Event
An impact event is a collision between astronomical objects causing measurable effects. Impact events have physical consequences and have been found to regularly occur in planetary systems, though the most frequent involve asteroids, comets or meteoroids and have minimal effect. When large objects impact terrestrial planets such as the Earth, there can be significant physical and biospheric consequences, though atmospheres mitigate many surface impacts through atmospheric entry. Impact craters and Impact structure, structures are dominant landforms on many of the Solar System's solid objects and present the strongest empirical evidence for their frequency and scale. Impact events appear to have played a significant role in the Formation and evolution of the Solar System, evolution of the Solar System since its formation. Major impact events have significantly shaped History of the Earth, Earth's history, and have been implicated in the giant impact theory, formation of the Earth†... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Craters On Mars
__NOTOC__ This is a list of craters on Mars. Impact craters on Mars larger than exist by the hundreds of thousands, but only about one thousand of them have names. Names are assigned by the International Astronomical Union after petitioning by relevant scientists, and in general, only craters that have a significant research interest are given names. Martian craters are named after famous scientists and science fiction authors, or if less than in diameter, after towns on Earth. Craters cannot be named for living people, and names for small craters are rarely intended to commemorate a specific town. Latitude and longitude are given as planetographic coordinates with west longitude. Catalog of named craters The catalog is divided into three partial lists: * List of craters on Mars: A–G * List of craters on Mars: H–N * List of craters on Mars: O–Z Names are grouped into tables for each letter of the alphabet, containing the crater's name (linked if article exists), co ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Ore Resources On Mars
Mars may contain ores that would be very useful to colonization of Mars, potential colonists. The abundance of volcanic features together with widespread cratering are strong evidence for a variety of ores. While nothing may be found on Mars that would justify the high cost of transport to Earth, the more ores that future colonists can obtain from Mars, the easier it would be to build colonies there. How deposits are made Ore deposits are produced with the help of large amounts of heat. On Mars, heat can come from molten rock moving under the ground and from crater impacts. Liquid rock under the ground is called magma. When magma sits in underground chambers, slowly cooling over thousands of years, heavier elements sink. These elements, including copper, chromium, iron, and nickel become concentrated at the bottom. When magma is hot, many elements are free to move. As cooling proceeds, the elements bind with each other to form chemical compounds or minerals. Because some elemen ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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