query: Where is the volcano Olympus Mons located?

title: Olympus Mons

text: several large lobes. Northwest of the volcano, the aureole extends a distance of up to and is known as Lycus Sulci (). East of Olympus Mons, the aureole is partially covered by lava flows, but where it is exposed it goes by different names (Gigas Sulci, for example). The origin of the aureole remains debated, but it was likely formed by huge landslides or gravity-driven thrust sheets that sloughed off the edges of the Olympus Mons shield. Olympus Mons Olympus Mons (; Latin for Mount Olympus) is a very large shield volcano on the planet Mars. The volcano has a

title: Olympus Mons

text: Olympus Mons Olympus Mons (; Latin for Mount Olympus) is a very large shield volcano on the planet Mars. The volcano has a height of nearly 25 km (13.6 mi or 72,000 ft) as measured by the Mars Orbiter Laser Altimeter (MOLA). Olympus Mons is about two and a half times Mount Everest's height above sea level. It is the largest volcano, the tallest planetary mountain, and the second tallest mountain in the Solar System compared to Rheasilvia on Vesta. It is the youngest of the large volcanoes on Mars, having formed during Mars's Hesperian Period. It had been known

title: Olympus Mons

text: is supported by a thick lithosphere. The extraordinary size of Olympus Mons is likely because Mars lacks mobile tectonic plates. Unlike on Earth, the crust of Mars remains fixed over a stationary hotspot, and a volcano can continue to discharge lava until it reaches an enormous height. Being a shield volcano, Olympus Mons has a very gently sloping profile. The average slope on the volcano's flanks is only 5°. Slopes are steepest near the middle part of the flanks and grow shallower toward the base, giving the flanks a concave upward profile. The shape of Olympus Mons is distinctly asymmetrical

title: Olympus Mons

text: Mons aureole deposits (discussed below). Olympus Mons lies at the edge of the Tharsis bulge, an ancient vast volcanic plateau likely formed by the end of the Noachian Period. During the Hesperian, when Olympus Mons began to form, the volcano was located on a shallow slope that descended from the high in Tharsis into the northern lowland basins. Over time, these basins received large volumes of sediment eroded from Tharsis and the southern highlands. The sediments likely contained abundant Noachian-aged phyllosilicates (clays) formed during an early period on Mars when surface water was abundant, and were thickest in the northwest

title: Olympus Mons

text: orbit around Mars in 1971 during a global dust-storm. The first objects to become visible as the dust began to settle, the tops of the Tharsis volcanoes, demonstrated that the altitude of these features greatly exceeded that of any mountain found on Earth, as astronomers expected. Observations of the planet from Mariner 9 confirmed that Nix Olympica was a volcano. Ultimately, astronomers adopted the name "Olympus Mons" for the albedo feature known as Nix Olympica. Olympus Mons is located between the northwestern edge of the Tharsis region and the eastern edge of Amazonis Planitia. It stands about from the other

title: Olympus Mons

text: the -diameter Pangboche crater (). The craters are notable for being two of several suspected source areas for shergottites, the most abundant class of Martian meteorites. As a shield volcano, Olympus Mons resembles the shape of the large volcanoes making up the Hawaiian Islands. The edifice is about wide. Because the mountain is so large, with complex structure at its edges, allocating a height to it is difficult. Olympus Mons stands above the Mars global datum, and its local relief, from the foot of the cliffs which form its northwest margin to its peak, is nearly (a little over twice

title: Olympus Mons

text: to astronomers since the late 19th century as the albedo feature Nix Olympica (Latin for "Olympic Snow"). Its mountainous nature was suspected well before space probes confirmed its identity as a mountain. The volcano is located in Mars's western hemisphere at approximately , just off the northwestern edge of the Tharsis bulge. The western portion of the volcano lies in the Amazonis quadrangle (MC-8) and the central and eastern portions in the adjoining Tharsis quadrangle (MC-9). Two impact craters on Olympus Mons have been assigned provisional names by the International Astronomical Union. They are the -diameter Karzok crater () and

title: Olympus Mons

text: and hence lead to the low gradients on the surface of the planet. Olympus Mons is an unlikely landing location for automated space probes in the near future. The high elevations preclude parachute-assisted landings because the atmosphere is insufficiently dense to slow the spacecraft down. Moreover, Olympus Mons stands in one of the dustiest regions of Mars. A mantle of fine dust obscures the underlying bedrock, possibly making rock samples hard to come by and likely posing a significant obstacle for rovers. Olympus Mons is the result of many thousands of highly fluid, basaltic lava flows that poured from volcanic

title: Alba Mons

text: Alba Mons Alba Mons (formerly known as Alba Patera, a term that has since been restricted to the volcano's summit caldera) is an immense, low-lying volcano located in the northern Tharsis region of the planet Mars. It is the largest volcano on Mars in terms of area, with volcanic flow fields that extend for at least from its summit. Although the volcano has a span comparable to that of the United States, it reaches an elevation of only at its highest point. This is about one-third the height of Olympus Mons, the tallest volcano on the planet. The flanks of

title: Alba Mons

title: Arsia Mons

text: Arsia Mons Arsia Mons is the southernmost of three volcanos (collectively known as Tharsis Montes) on the Tharsis bulge near the equator of the planet Mars. To its north is Pavonis Mons, and north of that is Ascraeus Mons. The tallest volcano in the solar system, Olympus Mons, is to its northwest. Its name comes from a corresponding albedo feature on a map by Giovanni Schiaparelli, which he named in turn after the legendary Roman forest of Arsia Silva. Arsia Mons is a shield volcano with a relatively low slope and a massive caldera at its summit. The southernmost of

title: Arsia Mons

text: of the features shows sunlight illuminating a side wall, suggesting that it may simply be a vertical pit rather than an entrance to a larger underground space. Nonetheless, the darkness of this feature implies that it must be at least 178 meters deep. Arsia Mons Arsia Mons is the southernmost of three volcanos (collectively known as Tharsis Montes) on the Tharsis bulge near the equator of the planet Mars. To its north is Pavonis Mons, and north of that is Ascraeus Mons. The tallest volcano in the solar system, Olympus Mons, is to its northwest. Its name comes from a

title: Pavonis Mons

text: a space elevator location, especially in science fiction. Pavonis Mons stands at the southern edge of the Tharsis quadrangle - approximately 400 km southwest of Ascraeus Mons (the northernmost of the Tharsis Montes) and 400 km northeast of Arsia Mons (the southernmost member of the chain). The Tharsis Montes volcanoes lie along the crest of a northeast-trending rise (Tharsis bulge) that extends more than 3,000 km across the western equatorial region of Mars. Olympus Mons, the largest volcano in the Solar System lies at the edge of the Tharsis bulge, about 1,200 km northwest of Pavonis Mons. Pavonis Mons is

title: Olympus Mons

text: Martian surface atmospheric pressure is less than one percent of Earth's, the much lower gravity of Mars increases the atmosphere's scale height; in other words, Mars's atmosphere is expansive and does not drop off in density with height as sharply as Earth's. The composition of Olympus Mons is approximately 44% silicates, 17.5% iron oxides (which give the planet its red coloration) 7% aluminum, 6% magnesium, 6% calcium, and particularly high proportions of sulfur oxide with 7%. These results point to the surface being largely composed of basalts and other mafic rocks, which would have erupted as low viscosity lava flows

title: Volcano

text: not present on Earth occur as well. Changes in the planet's atmosphere and observations of lightning have been attributed to ongoing volcanic eruptions, although there is no confirmation of whether or not Venus is still volcanically active. However, radar sounding by the Magellan probe revealed evidence for comparatively recent volcanic activity at Venus's highest volcano Maat Mons, in the form of ash flows near the summit and on the northern flank. There are several extinct volcanoes on Mars, four of which are vast shield volcanoes far bigger than any on Earth. They include Arsia Mons, Ascraeus Mons, Hecates Tholus, Olympus

title: Olympus Mons

text: the height of Mauna Kea as measured from its base on the ocean floor). The total elevation change from the plains of Amazonis Planitia, over to the northwest, to the summit approaches . The summit of the mountain has six nested calderas (collapsed craters) forming an irregular depression × across and up to deep. The volcano's outer edge consists of an escarpment, or cliff, up to tall (although obscured by lava flows in places), a feature unique among the shield volcanoes of Mars. Olympus Mons covers an area of about , which is approximately the size of Italy, and it

title: Olympus Mons

text: vents over a long period of time (The Hawaiian Islands exemplify similar shield volcanoes on a smaller scale – see Mauna Kea). Like the basalt volcanoes on Earth, Martian basaltic volcanoes are capable of erupting enormous quantities of ash. Due to the reduced gravity of Mars compared to Earth, there are lesser buoyant forces on the magma rising out of the crust. In addition, the magma chambers are thought to be much larger and deeper than the ones found on Earth. The flanks of Olympus Mons are made up of innumerable lava flows and channels. Many of the flows have

title: Olympus Mons

text: levees along their margins (pictured). The cooler, outer margins of the flow solidify, leaving a central trough of molten, flowing lava. Partially collapsed lava tubes are visible as chains of pit craters, and broad lava fans formed by lava emerging from intact, subsurface tubes are also common. In places along the volcano's base, solidified lava flows can be seen spilling out into the surrounding plains, forming broad aprons, and burying the basal escarpment. Crater counts from high-resolution images taken by the Mars Express orbiter in 2004 indicate that lava flows on the northwestern flank of Olympus Mons range in age

title: Elysium Mons

text: Elysium Mons Elysium Mons is a volcano on Mars located in the volcanic province Elysium, at , in the Martian eastern hemisphere. It stands about above the surrounding lava plains, and about above the Martian "datum". Its diameter is about , with a summit caldera about across. It is flanked by the smaller volcanoes Hecates Tholus to the northeast, and Albor Tholus to the southeast. Elysium Mons was discovered in 1972 in images returned by the Mariner 9 orbiter. The terrestrial volcano Emi Koussi (in Chad) has been studied as an analog of Elysium Mons. The two shield volcanoes have

title: Ascraeus Mons

text: crater Poynting is located 300 km to the west-southwest. Ascraeus Mons is roughly 480 km in diameter and is the second highest mountain on Mars, with a summit elevation of 18.1 km. The volcano has a very low profile with an average flank slope of 7°. Slopes are steepest in the middle portion of the flanks, flattening out toward the base and near the top where a broad summit plateau and caldera (collapse crater) complex are located. Volcanic vents, located on the northeastern and southwestern edges of the volcano, are sources for broad lava aprons, or fans, that bury nearby

title: Ascraeus Mons

text: Ascraeus Mons Ascraeus Mons is a large shield volcano located in the Tharsis region of the planet Mars. It is the northernmost and tallest of three shield volcanoes collectively known as the Tharsis Montes. The volcano's location corresponds to the classical albedo feature Ascraeus Lacus. Ascraeus Mons was discovered by the Mariner 9 spacecraft in 1971. The volcano was originally called North Spot because it was the northernmost of only four spots visible on the surface due to a global dust storm that was then enshrouding the planet. As the dust cleared, the spots were revealed to be extremely tall

title: Pavonis Mons

text: Pavonis Mons Pavonis Mons (Latin for "peacock mountain") is a large shield volcano located in the Tharsis region of the planet Mars. It is the middle member of a chain of three volcanic mountains (collectively known as the Tharsis Montes) that straddle the Martian equator between longitudes 235°E and 259°E. The volcano was discovered by the Mariner 9 spacecraft in 1971 and was originally called Middle Spot. Its name formally became Pavonis Mons in 1973. The equatorial location of its peak and its height make it the ideal terminus for a space elevator, and it has often been proposed as

title: Elysium Mons

text: the crater dimensions suggest a growth rate of the source volcano during that interval of 0.4–0.7 m per Ma, far slower than would be expected for a terrestrial volcano. This implies that Martian volcanism had slowed greatly by that point in history. Elysium Mons Elysium Mons is a volcano on Mars located in the volcanic province Elysium, at , in the Martian eastern hemisphere. It stands about above the surrounding lava plains, and about above the Martian "datum". Its diameter is about , with a summit caldera about across. It is flanked by the smaller volcanoes Hecates Tholus to the

title: Tharsis

text: the huge Olympus Mons and the Tharsis Montes are merely summit cones or parasitic cones on a much larger volcanic edifice. Tharsis Tharsis is a vast volcanic plateau centered near the equator in the western hemisphere of Mars. The region is home to the largest volcanoes in the Solar System, including the three enormous shield volcanoes Arsia Mons, Pavonis Mons, and Ascraeus Mons, which are collectively known as the Tharsis Montes. The tallest volcano on the planet, Olympus Mons, is often associated with the Tharsis region but is actually located off the western edge of the plateau. The name Tharsis

title: Hadriacus Mons

text: by a contact between magma and groundwater. "Hadriaca Patera", a term formerly used for the entire edifice, is now only used for the central caldera, which is in diameter. Hadriacus Mons Hadriacus Mons is an ancient, low-relief volcanic mountain on the planet Mars, located in the southern hemisphere just northeast of the impact basin Hellas and southwest of the similar volcano Tyrrhenus Mons. Hadriacus Mons is in the Hellas quadrangle. It has a diameter of . The name was approved in 2007. The flanks of Hadriacus Mons have been eroded into gullies; its southern slopes are incised by the outflow

title: Hadriacus Mons

text: Hadriacus Mons Hadriacus Mons is an ancient, low-relief volcanic mountain on the planet Mars, located in the southern hemisphere just northeast of the impact basin Hellas and southwest of the similar volcano Tyrrhenus Mons. Hadriacus Mons is in the Hellas quadrangle. It has a diameter of . The name was approved in 2007. The flanks of Hadriacus Mons have been eroded into gullies; its southern slopes are incised by the outflow channel Dao Vallis. The large extent of volcanic deposits and the caldera size leads some researchers to suggest that these features were the result of an explosive event caused

title: Pavonis Mons

text: bulge near the equator of the planet Mars. The other Tharsis volcanoes are Ascraeus Mons and Arsia Mons. The three Tharsis Montes, together with some smaller volcanoes to the north, form a fairly straight line. It has been proposed that this straight line of volcanoes is the result of the sort of plate motion which on Earth makes chains of "hot spot" volcanoes. Pavonis Mons Pavonis Mons (Latin for "peacock mountain") is a large shield volcano located in the Tharsis region of the planet Mars. It is the middle member of a chain of three volcanic mountains (collectively known as

title: Tharsis quadrangle

text: Mount Everest and about as big in area as all of Europe. Tharsis contains a group of large volcanoes. Olympus Mons is the tallest. Tharsis is a land of great volcanoes. Olympus Mons is the tallest known volcano in the Solar System; it is 100 times larger than any volcano on Earth. Ascraeus Mons and Pavonis Mons are at least 200 miles across and are over six miles above the plateau that they sit on—and, the plateau is three to four miles above the zero altitude of Mars. Pavonis Mons, the middle in a line of three volcanoes, sits at

title: Tyrrhenus Mons

text: apart. Voids were formed, then material fell into them, leaving holes. It is one of the oldest volcanoes on Mars. As a consequence of its old age, Tyrrhenus Mons has many radiating gullies on its slope. When it was formed, magma may have gone through frozen ground and then erupted as easily eroded ash, instead of lava flows. Tyrrhenus Mons Tyrrhenus Mons, formerly Tyrrhena Mons or Tyrrhena Patera, is a large volcano in the Mare Tyrrhenum quadrangle of Mars, located at 21.36° south latitude and 253.47° west longitude. The name "Tyrrhena Patera" now refers only to the central depression, a

title: Ascraeus Mons

text: volcanoes whose summits had projected above the dust-laden, lower atmosphere. The volcano's location corresponds to the classical albedo feature Ascraeus Lacus. The name comes from "Ascra," the birthplace of Hesiod. The word ascraeus is poetic for rural. The volcano's name officially became Ascraeus Mons in 1973. The volcano is located in the southeast-central portion of the Tharsis quadrangle at 11.8°N, 255.5°E in Mars' western hemisphere. A group of three smaller volcanoes (the Ceraunius-Uranius group) lies about 700 km to the northeast, and Pavonis Mons (the middle volcano of the Tharsis Montes) lies 500 km to the southwest. The 70-km diameter

title: Tyrrhenus Mons

text: Tyrrhenus Mons Tyrrhenus Mons, formerly Tyrrhena Mons or Tyrrhena Patera, is a large volcano in the Mare Tyrrhenum quadrangle of Mars, located at 21.36° south latitude and 253.47° west longitude. The name "Tyrrhena Patera" now refers only to the central depression, a volcanic crater or caldera. It was named after a classical albedo feature name. Pit chains are found at the summit of Tyrrhenus Mons. They are formed by collapse of material into underground voids. Since they form chains and concentric fractures that are aligned, they are probably caused by extension of the surface. Volcanic processes made the crust pull

title: Apollinaris Mons

text: Apollinaris Mons Apollinaris Mons is an ancient shield volcano in the southern hemisphere of Mars. It is situated near the equator, south of Elysium Planitia and north of Gusev crater. Elysium Planitia separates it from the volcanic province of Elysium to its northwest. The volcano's caldera is named Apollinaris Patera; this name formerly applied to the whole edifice. Apollinaris Mons is about 5 kilometres high with a base about 296 kilometres in diameter. On the top of this volcano is a caldera about 80 km (50 miles) in diameter. The volcano is approximately 3 billion to 3.5 billion years old.

title: Ascraeus Mons

text: period of high obliquity. During periods of high obliquity (axial tilt) the polar regions receive higher levels of sunlight. More water from the poles enters the atmosphere and condenses as ice or snowfall in the cooler equatorial regions. Mars changes its obliquity from about 15° to 35° in cycles of 120,000 years. Ascraeus Mons Ascraeus Mons is a large shield volcano located in the Tharsis region of the planet Mars. It is the northernmost and tallest of three shield volcanoes collectively known as the Tharsis Montes. The volcano's location corresponds to the classical albedo feature Ascraeus Lacus. Ascraeus Mons was

title: Mars

text: this, there are far fewer craters on Mars compared with the Moon, because the atmosphere of Mars provides protection against small meteors and surface modifying processes have erased some craters. Martian craters can have a morphology that suggests the ground became wet after the meteor impacted. The shield volcano Olympus Mons ("Mount Olympus") is an extinct volcano in the vast upland region Tharsis, which contains several other large volcanoes. Olympus Mons is roughly three times the height of Mount Everest, which in comparison stands at just over . It is either the tallest or second-tallest mountain in the Solar System,

title: Tharsis

text: Tharsis Tharsis is a vast volcanic plateau centered near the equator in the western hemisphere of Mars. The region is home to the largest volcanoes in the Solar System, including the three enormous shield volcanoes Arsia Mons, Pavonis Mons, and Ascraeus Mons, which are collectively known as the Tharsis Montes. The tallest volcano on the planet, Olympus Mons, is often associated with the Tharsis region but is actually located off the western edge of the plateau. The name Tharsis is the Greco-Latin transliteration of the biblical Tarshish, the land at the western extremity of the known world. Tharsis can have

title: Climate of Mars

text: CO geysers. Martian storms are significantly affected by Mars' large mountain ranges. Individual mountains like record holding Olympus Mons () can affect local weather but larger weather effects are due to the larger collection of volcanoes in the Tharsis region. One unique repeated weather phenomenon involving mountains is a spiral dust cloud that forms over Arsia Mons. The spiral dust cloud over Arsia Mons can tower above the volcano. Clouds are present around Arsia Mons throughout the Martian year, peaking in late summer. Clouds surrounding mountains display a seasonal variability. Clouds at Olympus Mons and Ascreaus Mons appear in northern

title: Apollinaris Mons

text: It was named in 1973 after a mountain spring near Rome in Italy. A study using a global climate model found that the Medusae Fossae Formation could have been formed from ash from Apollinaris Mons, Arsia Mons, and possibly Pavonis Mons. Apollinaris Mons Apollinaris Mons is an ancient shield volcano in the southern hemisphere of Mars. It is situated near the equator, south of Elysium Planitia and north of Gusev crater. Elysium Planitia separates it from the volcanic province of Elysium to its northwest. The volcano's caldera is named Apollinaris Patera; this name formerly applied to the whole edifice. Apollinaris

title: Volcanology of Mars

text: through the crust to produce volcanic mountains. However, the largest volcano on the planet, Olympus Mons, is thought to have formed when the plates were not moving. Olympus Mons may have formed just after the plate motion stopped. The mare-like plains on Mars are roughly 3 to 3.5 billion years old. The giant shield volcanoes are younger, formed between 1 and 2 billion years ago. Olympus Mons may be "as young as 200 million years." Norman H. Sleep, professor of geophysics at Stanford University, described how the three volcanoes that form a line along the Tharsis Ridge may be extinct

title: Alba Mons

text: last volcanic features to form were the small shield and caldera at the summit. Much later, between about 1,000 and 500 million years ago, a final stage of faulting occurred that may have been related to dike emplacement and the formation of pit crater chains. The classification of the Alba Mons volcano is uncertain. Some workers describe it as a shield volcano, others as a lowland patera (in contrast to highland paterae, which are low-lying ancient volcanoes with furrowed ash deposits located in the southern Martian highlands), and still others consider it a one-of-a-kind volcanic structure unique to Mars. Some

title: Alba Mons

text: majority of those in the southern highlands. This fact presents a problem for researchers who propose that valley networks were carved by rainfall runoff during an early, warm and wet period of Martian history. If the climate conditions changed billions of years ago into today's cold and dry Mars (where rainfall is impossible), how does one explain the younger valleys on Alba Mons? Did Alba's valley networks form differently from those in the highlands, and if so, how? Why do the valleys on Alba Mons occur mainly on the northern flanks of the volcano? These questions are still being debated.

title: Alba Mons

text: Alba Mons have very gentle slopes. The average slope along the volcano's northern (and steepest) flank is 0.5°, which is over five times lower than the slopes on the other large Tharsis volcanoes. In broad profile, Alba Mons resembles a vast but barely raised welt on the planet's surface. It is a unique volcanic structure with no counterpart on Earth or elsewhere on Mars. In addition to its great size and low relief, Alba Mons has a number of other distinguishing features. The central portion of the volcano is surrounded by an incomplete ring of faults (graben) and fractures, called

title: Mons (planetary nomenclature)

text: round mountains found on Venus get names with the term "farrum". The term "mons", like other terms of planetary nomenclature, describes only the external view of the feature, but not its origin or geological structure. It is used for mountains of any origin, and objects in this class are very diverse. Usually they are results of tectonic, impact or volcanic processes. Examples of such mountains are the Maxwell Montes on Venus, the Montes Apenninus on the Moon and Olympus Mons on Mars, respectively. More unusual origins are also possible. For example, the Geryon Montes of Mars are an erosional remnant

title: Mons Huygens

text: Mons Huygens Mons Huygens is the Moon's tallest mountain (but not its highest point). It is about high and is located in the Montes Apenninus. The Montes Apenninus were formed by the impact that created Mare Imbrium. Adjacent is Mons Ampère to the west. Further west is the crater Huxley. The mountain was named after the Dutch astronomer, mathematician and physician Christiaan Huygens, it was officially named by the IAU in 1961. Mons Huygens is high, about the same height as Aeolis Mons located on Mars in the middle of Gale crater, and taller than Mons Hadley located on the

title: Pavonis Mons

text: the smallest of the Tharsis Montes volcanoes, measuring about 375 km across and standing 14 km above Mars' mean surface level. As a shield volcano, Pavonis Mons has an extremely low profile with flank slopes that average only 4°. The summit contains a deep, circular caldera that is 47 km in diameter and almost 5 km deep. A larger, shallower depression lies immediately northeast of the smaller caldera. The large depression is about 90 km in diameter and structurally more complex than the small caldera. Like most of the Tharsis region, Pavonis Mons has a high albedo (reflectivity) and low

title: Alba Mons

text: portions of Alba’s surface may contain a higher abundance of duricrusts, sand, and rocks compared to the rest of the volcano. High thermal inertia can also indicate the presence of exposed water ice. Theoretical models of water-equivalent hydrogen (WEH) from epithermal neutrons detected by the Mars Odyssey Neutron Spectrometer (MONS) instrument suggest that the regolith just below the surface on Alba's northern flank may contain 7.6% WEH by mass. This concentration could indicate water present as remnant ice or in hydrated minerals. Alba Mons is one of several areas on the planet that may contain thick deposits of near-surface ice

title: Ascraeus Mons

text: surrounded by lava flow plains that are mid to late Amazonian in age. The elevation of the plains averages about 3 km above datum (Martian "sea" level), giving the volcano an average vertical relief of 15 km. However, the elevation of the plains varies considerably. The plains northwest of the volcano are less than 2 km in elevation. The plains are highest (>3 km) southeast of the volcano. The lava plains northwest of Ascraeus Mons are notable for having two dark collapse pits photographed by the HiRISE camera on the Mars Reconnaissance Orbiter (MRO) in November 2010 (pictured in gallery

title: Alba Mons

text: of at least 5.7 million km and has a volume of about 2.5 million km. The volcano dominates the northern portion of the Tharsis bulge and is so large and geologically distinct that it can almost be treated as an entire volcanic province unto itself. Although Alba Mons reaches a maximum elevation of above Mars’ datum, the elevation difference between its summit and surrounding terrain (relief) is much greater on the north side of the volcano (about ) compared to the south side (about ). The reason for this asymmetry is that Alba straddles the dichotomy boundary between the cratered

title: Call of Duty: Infinite Warfare

text: AATIS guns, and kills himself to trigger the beacon. The main SDF arrives and the "Olympus Mons" destroys UNSA headquarters, killing Admiral Raines. With no other options, Reyes decides to use the opportunity to board and commandeer the "Olympus Mons". He manages to battle his way to the bridge and kill Admiral Kotch. He then has the "Olympus Mons" travel back to Mars, where he intends to use the ship to destroy the SDF's orbital shipyard and cripple their fleet in return. While the "Olympus Mons" and "Retribution" manage to destroy many SDF ships, the "Olympus Mons" suffers too much

title: Pettit (Martian crater)

text: Pettit (Martian crater) Pettit Crater is a crater in the Amazonis quadrangle of Mars, located at 12.39° north latitude and 173.87° west longitude. Pettit lies west of the giant volcano Olympus Mons. It is 92.49 km in diameter and was named after Edison Pettit, an American astronomer (1890–1962). No major craters are located nearby but some smaller ones as the area's surface is young west is the large and wide but low Marte Vallis, also in the west are Tartarus Colles and the noted Orcus Patera. Around 250 km west is the 180th meridian marking the furthermost areas of the

title: Pettit (Martian crater)

text: planet, west of that is the Elysium quadrangle. Pettit has a circular central peak in the middle, the peak features dark slope streaks. Pettit (Martian crater) Pettit Crater is a crater in the Amazonis quadrangle of Mars, located at 12.39° north latitude and 173.87° west longitude. Pettit lies west of the giant volcano Olympus Mons. It is 92.49 km in diameter and was named after Edison Pettit, an American astronomer (1890–1962). No major craters are located nearby but some smaller ones as the area's surface is young west is the large and wide but low Marte Vallis, also in the

title: Olympus Mons

text: unaware of standing on a very high mountain, as the slope of the volcano would extend far beyond the horizon, a mere 3 kilometers away. The typical atmospheric pressure at the top of Olympus Mons is 72 pascals, about 12% of the average Martian surface pressure of 600 pascals. Both are exceedingly low by terrestrial standards; by comparison, the atmospheric pressure at the summit of Mount Everest is 32,000 pascals, or about 32% of Earth's sea level pressure. Even so, high-altitude orographic clouds frequently drift over the Olympus Mons summit, and airborne Martian dust is still present. Although the average

title: Olympus Mons

text: This inhibition of southeasterly basal spreading in Olympus Mons could account for the structural and topographic asymmetry of the mountain. Numerical models of particle dynamics involving lateral differences in friction along the base of Olympus Mons have been shown to reproduce the volcano's present shape and asymmetry fairly well. It has been speculated that the detachment along the weak layers was aided by the presence of high-pressure water in the sediment pore spaces, which would have interesting astrobiological implications. If water-saturated zones still exist in sediments under the volcano, they would likely have been kept warm by a high geothermal

title: Olympus Mons

text: three large Martian shield volcanoes, collectively called the Tharsis Montes (Arsia Mons, Pavonis Mons, and Ascraeus Mons). The Tharsis Montes are slightly smaller than Olympus Mons. A wide, annular depression or moat about deep surrounds the base of Olympus Mons and is thought to be due to the volcano's immense weight pressing down on the Martian crust. The depth of this depression is greater on the northwest side of the mountain than on the southeast side. Olympus Mons is partially surrounded by a region of distinctive grooved or corrugated terrain known as the Olympus Mons aureole. The aureole consists of

title: Olympus Mons

text: - its flanks are shallower and extend farther from the summit in the northwestern direction than they do to the southeast. The volcano's shape and profile have been likened to a "circus tent" held up by a single pole that is shifted off center. Due to the size and shallow slopes of Olympus Mons, an observer standing on the Martian surface would be unable to view the entire profile of the volcano, even from a great distance. The curvature of the planet and the volcano itself would obscure such a synoptic view. Similarly, an observer near the summit would be

title: Olympus Mons

text: gradient and residual heat from the volcano's magma chamber. Potential springs or seeps around the volcano would offer exciting possibilities for detecting microbial life. Olympus Mons and a few other volcanoes in the Tharsis region stand high enough to reach above the frequent Martian dust-storms recorded by telescopic observers as early as the 19th century. The astronomer Patrick Moore pointed out that Schiaparelli (1835–1910) "had found that his "Nodus Gordis" and "Olympic Snow" [Nix Olympica] were almost the only features to be seen" during dust storms, and "guessed correctly that they must be high". The Mariner 9 spacecraft arrived in

title: Olympus Mons

text: large lava lake. Using geometric relationships of caldera dimensions from laboratory models, scientists have estimated that the magma chamber associated with the largest caldera on Olympus Mons lies at a depth of about below the caldera floor. Crater size-frequency distributions on the caldera floors indicate the calderas range in age from 350 Mya to about 150 Mya. All probably formed within 100 million years of each other. Olympus Mons is asymmetrical structurally as well as topographically. The longer, more shallow northwestern flank displays extensional features, such as large slumps and normal faults. In contrast, the volcano's steeper southeastern side has

title: Arsia Mons

text: the three Tharsis Montes volcanoes, it is the only major Tharsis volcano south of the equator. The volcano is in diameter, almost high (more than higher than the surrounding plains), and the summit caldera is 110 km (72 miles) wide. It experiences atmospheric pressure lower than 107 pascals at the summit. Excluding Olympus Mons, it is the largest known volcano in terms of volume. Arsia Mons has 30 times the volume of Mauna Loa in Hawaii, the largest volcano on the Earth. The caldera of Arsia Mons was formed when the mountain collapsed in on itself after its reservoir of

title: Olympus Mons

text: extensional. A subterranean rift may develop at the base of the volcano, causing the underlying crust to spread apart. If the volcano rests on sediments containing mechanically weak layers (e.g., beds of water-saturated clay), detachment zones (decollements) may develop in the weak layers. The extensional stresses in the detachment zones can produce giant landslides and normal faults on the volcano's flanks, leading to the formation of a basal escarpment. Further from the volcano, these detachment zones can express themselves as a succession of overlapping, gravity driven thrust faults. This mechanism has long been cited as an explanation of the Olympus

title: Alba Mons

text: following withdrawal and depletion of a magma chamber after an eruption. Caldera dimensions allow scientists to infer the geometry and depth of the magma chamber beneath the summit of the volcano. The shallowness of Alba’s calderas compared to those seen on Olympus Mons and most of the other Tharsis volcanoes implies that Alba’s magma reservoir was wider and shallower than those of its neighbors. Most of the central edifice of Alba Mons is mantled with a layer of dust approximately thick. The dust layer is visible in high resolution images of the summit (pictured right). In places, the dust has

title: Ascraeus Mons

text: pattern. They are interpreted to be the surface expression of thrust faults that formed due to compression along the volcano's flanks. Flank terraces are also common on Olympus Mons and the other Tharsis shield volcanoes. The source of the compressive stresses is still debated. The flank terraces may be due to compressional failure of the volcano, flexing of the underlying lithosphere due to the volcano's massive weight, cycles of magma chamber inflation and deflation, or shallow gravitational slumping. Fissures, or flank vents, at the southwestern and northeastern edges of the volcano are the sources of the lava aprons that spread

title: Alba Mons

text: volcano). The IAU named the volcano Alba Patera in 1973. The volcano is often simply called Alba when the context is understood. Alba Mons is centered at in the Arcadia quadrangle (MC-3). Much of the volcano's western flank is located in the adjacent Diacria quadrangle (MC-2). Flows from the volcano can be found as far north as 61°N and as far south as 26°N (in the northern Tharsis quadrangle). If one takes the outer margin of the flows as the volcano's base, then Alba Mons has north–south dimensions of about and a maximum width of . It covers an area

title: Sapas Mons

text: Sapas Mons Sapas Mons is a large volcano located in the Atla Regio region of Venus. Sapas is named after the Canaanite sun goddess. It measures about across and high. Its flanks show numerous overlapping lava flows. The dark flows on the lower right of the radar image are thought to be smoother than the brighter ones near the central part of the volcano. Many of the flows appear to have been erupted along the flanks of the volcano rather than from the double summit. This type of flank eruption is common on large volcanoes on Earth, such as the

title: Maat Mons

text: variation in the concentrations of sulfur dioxide (SO) and methane (CH) in Venus' middle and upper atmosphere. One possible explanation for this was the injection of volcanic gases into the atmosphere by plinian eruptions at Maat Mons. More recent studies have suggested that the volcano structure, distribution of lava flows, pit craters, summit morphology, and other small-scale features are indicative of recent volcanic activity on Maat Mons. Although many lines of evidence suggest that Venus is likely to be volcanically active, present-day eruptions at Maat Mons have not been confirmed. Maat Mons Maat Mons is a massive shield volcano. It

title: Maat Mons

text: Maat Mons Maat Mons is a massive shield volcano. It is the second-highest mountain, and the highest volcano, on the planet Venus. It rises above the mean planetary radius at , and nearly 5 km above the surrounding plains. It is named after the Egyptian goddess of truth and justice, Ma'at. Maat Mons has a large summit caldera, 28×31 km in size. Within the large caldera there are at least five smaller collapse craters, up to 10 km in diameter. A chain of small craters 3–5 km in diameter extends some 40 km along the southeast flank of the volcano,

title: Alba Mons

text: valley networks on the north side of the volcano is that they were produced through sapping or melting of ice-rich dust deposited during a relatively recent, Amazonian-aged glacial epoch. In summary, current geologic analysis of Alba Mons suggests that the volcano was built by lavas with rheological properties similar to basalts. If early explosive activity happened at Alba Mons, the evidence (in the form of extensive ash deposits) is largely buried by younger basaltic lavas. The immense system of fractures surrounding Alba Mons is perhaps the most striking feature of the volcano. The fractures are tectonic features indicating stresses in

title: Sapas Mons

text: be composed of at least five large volcanoes such as Sapas Mons, which are commonly linked by complex systems of fractures or rift zones. If comparable to similar features on Earth, Atla Regio probably formed when large volumes of molten rock upwelled from areas within the interior of Venus known as 'hot spots.' Sapas Mons Sapas Mons is a large volcano located in the Atla Regio region of Venus. Sapas is named after the Canaanite sun goddess. It measures about across and high. Its flanks show numerous overlapping lava flows. The dark flows on the lower right of the radar

title: Olympus Mons

text: features indicating compression, including step-like terraces in the volcano's mid-flank region (interpreted as thrust faults) and a number of wrinkle ridges located at the basal escarpment. Why opposite sides of the mountain should show different styles of deformation may lie in how large shield volcanoes grow laterally and in how variations within the volcanic substrate have affected the mountain's final shape. Large shield volcanoes grow not only by adding material to their flanks as erupted lava, but also by spreading laterally at their bases. As a volcano grows in size, the stress field underneath the volcano changes from compressional to

title: Ushas Mons

text: on this type of volcano on Venus, and is believed to result from a large zone of hot material upwelling from the Venusian mantle, a phenomenon known on Earth as a "hotspot." Ushas Mons Ushas Mons is a 2-kilometer-high (1.25 mile) volcano in the southern hemisphere of Venus at 25 degrees south latitude, 323 degrees east longitude. Its name is derived from vedic goddess of dawn Ushas The volcano is marked by numerous bright lava flows and a set of north-south trending fractures, many of which appear to have formed after the lavas were erupted onto the surface. In the

title: Ascraeus Mons

text: zone of knobby terrain outlined by a semicircular zone of concentric ridges. Similar deposits are also found at the northwestern edges of the other two Tharsis Montes, Pavonis Mons and Arsia Mons, as well as on Olympus Mons. The FSD at Ascraeus Mons is the smallest of those on the Tharsis Montes, covering an area of 14,000 km and extending outward from the volcano's base for about 100 km. The origin of these deposits has been debated for decades. However, recent geologic evidence suggests that FSDs are deposits left by glaciers, which covered portions of the volcanoes during a recent

title: Alba Mons

text: runoff. Alba Mons has some of the oldest, extensively exposed volcanic deposits in the Tharsis region. Geologic evidence indicates that significant volcanic activity ended much earlier at Alba Mons than at Olympus Mons and the Tharsis Montes volcanoes. Volcanic deposits from Alba Mons range in age from Hesperian to early Amazonian (approximately 3600 to 3200 million years old). For years the volcano's formal name was Alba Patera. "Patera" (pl. "paterae") is Latin for a shallow drinking bowl or saucer. The term was applied to certain ill-defined, scalloped-edged craters that appeared in early spacecraft images to be volcanic (or non-impact) in

title: Irnini Mons

text: Patera depression at the summit. The volcano is crossed by various rift zones, including the north-south trending Badb Linea rift, the Guor Linea rift extending to the northwest, and the Virtus Linea rift continuing to the southeast. The combination of volcanic-tectonic structures around Irnini Mons supports varying intensities of deformation and a multi-directional stress history. Although classified as a shield volcano, Irnini Mons contains many elements of the Venusian coronae, bringing speculation to its formation. If Irnini Mons was originally a corona, a shallow oval-shaped depression, it would support a thin lithosphere on Venus. On the other hand, it being

title: Ushas Mons

text: Ushas Mons Ushas Mons is a 2-kilometer-high (1.25 mile) volcano in the southern hemisphere of Venus at 25 degrees south latitude, 323 degrees east longitude. Its name is derived from vedic goddess of dawn Ushas The volcano is marked by numerous bright lava flows and a set of north-south trending fractures, many of which appear to have formed after the lavas were erupted onto the surface. In the central summit area, however, younger flows remain unfractured. An impact crater can be seen among the fractures in the upper center of the image. The association of faulting and volcanism is common

title: Ascraeus Mons

text: portions of the volcano and extend over 100 km out into the surrounding plains. The southwest-northeast orientation of the aprons matches the orientation of the Tharsis Montes, suggesting that a major fissure or rift in the Martian crust is responsible for the orientation of both the aprons and the Tharsis Montes chain. The presence of the lava aprons causes some disagreement in the actual dimensions of the volcano. If the aprons are included as part of the edifice then Ascraeus Mons has dimensions closer to 375 × 870 km. Like most of the Tharsis region, Ascraeus Mons has a high

title: Irnini Mons

text: uplift theory is correct, then most of the topographic highs in the Eistla Regio region of Venus would also be due to uplift. Additionally, it supports the hypothesis of a thin lithosphere on Venus. The theory of corona uplift much more unlikely than Irnini Mons simply being a shield volcano which underwent natural volcanic progression. An approximate timeline of the regional geologic events, occurring over a time period of a few hundred million years, can be summarized as: Irnini Mons Irnini Mons is a volcanic structure on the planet Venus, and is named after the Assyro-Babylonian goddess of cedar-tree mountains.

title: Ascraeus Mons

text: This could indicate that the lava flows on the flanks of Ascraeus Mons consist of rough Aā-type flows, a conclusion supported by photogeologic analysis of lava flow morphologies. The flanks of Ascraeus Mons have a rumpled appearance caused by numerous low, rounded terrace-like structures arranged concentrically around the summit of the volcano. The terraces are spaced 30 to 50 km apart, have lengths up to 100 km, radial widths of 30 km, and heights of about 3 km. Individual terraces are not continuous around the volcano, but instead consist of arcuate segments that overlap with each other, forming an imbricate

title: Irnini Mons

text: proximity to its "pressurized hole". Circumferential ridges and graben are also highly reflective to radar, and therefore, easily observed around the Sappho Patera depression. These concentric features formed after Irnini Mons lost the high pressure dynamic support from the mantle upwelling due to the lack of overlying flows. The presence of circumferential structures along a shallow depression on Irnini Mons' summit is a characteristic of coronae on Venus. The presence of corona-like features suggest two possible theories for interpretation of how Irnini Mons developed. One hypothesis is a transition from a primarily shield volcano structure to a primarily corona structure

title: Alba Mons

text: of volcanic activity at Alba Mons probably involved massive effusive eruptions of low viscosity lavas that formed the volcano's broad, flat apron. Lava flows of the apron unit straddle the early Hesperian-late Hesperian boundary, having erupted approximately 3700 to 3500 million years ago. The middle unit, which is early Amazonian in age, makes up the flanks of the main Alba edifice and records a time of more focused effusive activity consisting of long tube- and channel-fed flows. Volcanic spreading occurred in a northward direction forming the two flanking lobes. (See Olympus Mons and Tharsis for a discussion of volcanic spreading

title: Olympus Mons

text: where basin depth was greatest. As the volcano grew through lateral spreading, low-friction detachment zones preferentially developed in the thicker sediment layers to the northwest, creating the basal escarpment and widespread lobes of aureole material (Lycus Sulci). Spreading also occurred to the southeast; however, it was more constrained in that direction by the Tharsis rise, which presented a higher-friction zone at the volcano's base. Friction was higher in that direction because the sediments were thinner and probably consisted of coarser grained material resistant to sliding. The competent and rugged basement rocks of Tharsis acted as an additional source of friction.

title: Irnini Mons

text: a shield volcano supports the theory of a thicker lithosphere and Irnini Mons' stress history could be summarized simply as a transition from predominantly compressive forces to extensional relaxation, resulting in the observed radiating graben and concentric ridges. Irnini Mons is a significant structural feature on Venus because the preservation of the geology allows for the analysis of Venus' regional stress orientation in response to a pressurized magma chamber over time. The geology of Irnini Mons and the surrounding region was interpreted using synthetic aperture radar data from the Magellan space mission. Stratigraphic units were identified using their relative brightness

title: Alba Mons

text: origin. In September 2007, the International Astronomical Union (IAU) renamed the volcano Alba Mons (Alba Mountain), reserving the term Alba Patera for the volcano's two central depressions (calderas). Nevertheless, the entire volcano is still commonly called Alba Patera in the planetary science literature. The term Alba is from the Latin word for white and refers to the clouds frequently seen over the region from Earth-based telescopes. The volcano was discovered by the Mariner 9 spacecraft in 1972 and was initially known as the Alba volcanic feature or the Arcadia Ring (in reference to the partial ring of fractures around the

title: Alba Mons

text: its lava flows and the geometry of the faults cutting its flanks. Surface features of the volcano, such as gullies and valley networks, have also been extensively studied. These efforts have the overall goal of deciphering the geologic history of the volcano and the volcano-tectonic processes involved in its formation. Such understanding can shed light on the nature and evolution of the Martian interior and the planet's climate history. Alba Mons is notable for the remarkable length, diversity, and crisp appearance of its lava flows. Many of the flows radiate from the summit, but others appear to originate from vents

title: Tharsis

text: long and includes most of the region covered by the Tharsis quadrangle and the northwestern portion of the adjoining Phoenicis Lacus quadrangle to the south. Finally, the massive Olympus Mons and its associated lava flows and aureole deposits form another distinct subprovince of the Tharsis region. This subregion is about 1600 km across. It lies off the main topographic bulge, but is clearly related to the volcanic processes that formed Tharsis. Olympus Mons is the youngest of the large Tharsis volcanoes. Tharsis is commonly called a volcano-tectonic province, meaning that it is the product of volcanism and associated tectonic processes

title: Mons

text: the 3rd Armored Division (United States), and is one of the largest gatherings of World War II tanks in the world. There are several public educational facilities in Mons: Mons is located along the N56 road. It is also accessed via European route E42, which is a continuation of French Autoroute A2, linking the British WW1 battlefields of Mons with the Somme Battlefields, Mons railway station opened on 19 December 1841. A small, general aviation airfield Saint-Ghislain Airport is located nearby for private aircraft. Mons has a typical Belgian oceanic climate with relatively narrow temperature differences between seasons for its

title: Ceraunius Tholus

text: Mons, and Pavonis Mons. Ceraunius Tholus may have even had its glaciers melt to form some temporary lakes in the past. The smoothness and flatness of the Ceraunius Tholus caldera floor suggests that in the past meltwater accumulated in a caldera lake. Ceraunius Tholus is on the Tharsis rise, also called the Tharsis bulge. Tharsis is a land of great volcanoes. Olympus Mons is the tallest known volcano. Ascraeus Mons and Pavonis Mons are at least 320 km across and are over 10 km above the plateau that they sit on. The plateau is five to four seven kilometers above

title: Ascraeus Mons

text: albedo (reflectivity) and low thermal inertia, indicating that the volcano and surrounding areas are covered with large amounts of fine dust. (See the Martian Surface.) The dust forms a mantle over the surface that obscures or mutes much of the fine-scale topography and geology of the region. Tharsis is probably dusty because of its high elevations. The atmospheric density is too low to mobilize and remove dust once it is deposited. The atmospheric pressure at the summit of Ascraeus Mons averages 100 pascal (1.0 mbar); this is only 17% of the average surface pressure of 600 pascal. Ascraeus Mons is

title: Anseris Mons

text: M. Antoniadi in 1930. The name was approved by the International Astronomical Union (IAU) in 1991. Anseris Mons is not a volcano. Geologically, the massif is thought to be the eroded remnant of an ancient crustal block uplifted from depths of several kilometers in the formation of the Hellas impact basin during the period of heavy bombardment. Anseris Mons is the type area for a large set of rugged mountain blocks (>25 km across) that occur in a relatively continuous band 200 to 500 km wide around the western, northeastern, eastern, and southeastern rim of the Hellas basin. Many of

title: Mons Claudianus

text: Mons Claudianus Mons Claudianus was a Roman quarry in the eastern desert of Egypt. It consisted of a garrison, a quarrying site, and civilian and workers' quarters. Granodiorite was mined for the Roman Empire where it was used as a building material. Mons Claudianus is located in the mountains of the Egyptian Eastern desert about midway between the Red Sea and Qena, in the present day Red Sea Governorate. Today tourists can see fragments of granite, with several artifacts such as a broken column. A number of texts written on broken pottery (ostraca) have been discovered at the site. Mons

title: Alba Mons

text: Calculated flow rates are also lower than originally thought, ranging from 10 to 1.3 million m per second. The lower range of eruption rates for Alba Mons is within the range of the highest terrestrial volcanic flows, such as the 1984 Mauna Loa, North Queensland (McBride Province), and the Columbia River basalts. The highest range is several orders of magnitude higher than the effusive rates for any terrestrial volcano. Since the late 1980s, some researchers have suspected that Alba Mons eruptions included a significant amount of pyroclastics (and therefore explosive activity) during early phases of its development. The evidence was

title: Doom Mons

text: Titan's outer crust. I speculate that the mountains might be a chain of volcanoes that oozed up along cracks in the crust after the impact." Doom Mons is named after Mount Doom, a volcano that appears in J. R. R. Tolkien's fictional world of Middle-earth, most prominently in "The Lord of the Rings". The name follows a convention by the IAU Working Group for Planetary System Nomenclature that Titanean mountains are named after mountains in Tolkien's works. Other examples of Titanean mountains or mountain ranges named after Tolkien's works include Erebor Mons, the Irensaga Montes, Mindolluin Montes, Misty Montes, Mithrim

title: Alba Mons

text: and fissures on the lower flanks of the volcano. Individual flows may exceed in length. Lava flows near the summit calderas appear to be significantly shorter and narrower than those on more distal parts of the volcano. The two most common types of volcanic flows on Alba Mons are sheet flows and tube-and-channel fed flows. Sheet flows (also called tabular flows) form multiple, overlapping lobes with steep margins. The flows typically lack central channels. They are flat-topped and generally about wide on the upper flanks of the volcano but become much wider and lobate toward their downstream (distal) ends. Most

title: Mons Vinogradov

text: Mons Vinogradov Mons Vinogradov is a rugged massif that is located on the lunar mare where Oceanus Procellarum to the southwest joins Mare Imbrium to the east. There are three primary peaks in this formation, which rise to altitudes of 1.0–1.4 km above the surface. To the east of this rise is the crater Euler, and to the southeast is an area of rugged ground that reaches the Montes Carpatus range. The Carpatus mountain range forms the southwest boundary of the Mare Imbrium. The selenographic coordinate of Mons Vinogradov is 22.4 N, 32.4 W, and it has a maximum diameter

title: Mons Vinogradov

text: of 25 km at the base. It was named after Aleksandr P. Vinogradov. This mountain was formerly named Euler Beta (β), or Mons Euler. In the rugged ground just to the southeast of this mountain is a set of tiny craters that have been assigned names by the IAU. These are listed in the table below. West of Natasha is a rille known as Rima Wan-Yu. South of the rim of Akis is Catena Pierre. Mons Vinogradov Mons Vinogradov is a rugged massif that is located on the lunar mare where Oceanus Procellarum to the southwest joins Mare Imbrium to

title: Alba Mons

text: tension cracks into which surface material has drained. The graben and fractures around Alba Mons (hereafter simply called faults unless otherwise indicated) occur in swarms that go by different names depending on their location with respect to Alba’s center. South of the volcano is a broad region of intensely fractured terrain called Ceraunius Fossae, which consists of roughly parallel arrays of narrow, north-south oriented faults. These faults diverge around the flanks of the volcano, forming an incomplete ring about in diameter. The set of faults on Alba's western flank is called Alba Fossae and the one on the eastern flank

title: Alba Mons

text: - wide. An individual ridge may have a discontinuous channel or line of pits that run along its crest. Tube- and channel-fed flows are particularly prominent on the western flank of the volcano where individual ridges can be traced for several hundred kilometers. The origin of the ridges is uncertain. They may form by successive buildup of solidified lava at the mouth of a channel or tube, with each pulse of flowing lava adding to the length of the ridge. In addition to the two main types of flows, numerous undifferentiated flows are present around Alba Mons that are either

title: Irnini Mons

text: volcanic-tectonic features that had developed over the life-span of the volcano. The transition from volcanic build-up to summit collapse is directly related to the degree of melting from the central magma chamber. An alternate theory is, rather than being a shield volcano, Irnini Mons developed as a corona under thin lithosphere, and was simply tectonically uplifted to its present elevation under the north-south compression. Coronae develop when a mantle upwelling bends the crust upwards, which later collapses when the dynamic support from the upwelling is lost, resulting in a shallow oval-shaped depression. This hypothesis requires two assumptions: If the corona

title: Irnini Mons

text: compression near the summit. The most widely accepted belief is that Irnini Mons formed as a shield volcano, and experienced a crater collapse later in its geologic life. Shield Volcanoes on Venus develop as a result of mantle upwelling occurring under thick lithosphere in a constant location over a relatively long period of time. Effusive flows from the magma chamber emitted low viscosity, basaltic lava which resurfaced the regional tessera plains of Venus. The placid flows eventually formed a shallow sloping volcano with its summit above the magma pressurized center. Radiating fractures and ridges due to compression formed simultaneously with

title: Olympus Mons

text: from 115 million years old (Mya) to only 2 Mya. These ages are very recent in geological terms, suggesting that the mountain may still be volcanically active, though in a very quiescent and episodic fashion. The caldera complex at the peak of the volcano is made of at least six overlapping calderas and caldera segments (pictured). Calderas are formed by roof collapse following depletion and withdrawal of the subsurface magma chamber after an eruption. Each caldera thus represents a separate pulse of volcanic activity on the mountain. The largest and oldest caldera segment appears to have formed as a single,

title: Athis-Mons

text: people were left homeless. Athis-Mons had to be entirely rebuilt after the war. Athis-Mons is located at the confluence of Orge and Seine rivers, and at the southern edge of the international airport of Orly. The canton of Athis-Mons has 2 communes (the other is Paray-Vieille-Poste) and 36,615 inhabitants. Athis-Mons is a twin town of Ballina in Ireland. Athis-Mons is served by Athis-Mons station on Paris RER line C. The commune has nine preschools ("écoles maternelles") and eight elementary schools ("écoles élémentaires"). There is a private Catholic school, . <BR> Athis-Mons Athis-Mons () is a commune in the southern suburbs

title: Mons Claudianus

text: Orientale, Documents de Fouilles 29). Nos. 1—190. Mons Claudianus Mons Claudianus was a Roman quarry in the eastern desert of Egypt. It consisted of a garrison, a quarrying site, and civilian and workers' quarters. Granodiorite was mined for the Roman Empire where it was used as a building material. Mons Claudianus is located in the mountains of the Egyptian Eastern desert about midway between the Red Sea and Qena, in the present day Red Sea Governorate. Today tourists can see fragments of granite, with several artifacts such as a broken column. A number of texts written on broken pottery (ostraca)

title: Ascraeus Mons

text: of Kilauea Volcano, Hawaii. In some cases, they may mark skylights/entrances to subsurface lava caves. Ascraeus Mons was built by many thousands of fluid basaltic lava flows. Except for its great size, it resembles terrestrial shield volcanoes like those that form the Hawaiian Islands. The flanks of Ascraeus Mons are covered with narrow, lobate lava flows and lava channels. Many of the lava flows have levees along their margins. Levees are parallel ridges formed at the edges of lava flows. The cooler, outer margins of the flow solidify, leaving a central trough of molten, flowing lava. Partially collapsed lava tubes