Tharsis quadrangle

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Tharsis quadrangle
USGS-Mars-MC-9-TharsisRegion-mola.png
Map of Tharsis quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are white and the lowest are blue.
Coordinates 15°00′N112°30′W / 15°N 112.5°W / 15; -112.5
Image of the Tharsis Quadrangle (MC-9). The region contains the Olympus Mons, Ascraeus Mons and Pavonis Mons, three of the four largest shield volanoes on Mars. The north-central part contains Ceraunius Fossae. PIA00169-MC-9-TharsisRegion-19980605.jpg
Image of the Tharsis Quadrangle (MC-9). The region contains the Olympus Mons, Ascraeus Mons and Pavonis Mons, three of the four largest shield volanoes on Mars. The north-central part contains Ceraunius Fossae.

The Tharsis quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Tharsis quadrangle is also referred to as MC-9 (Mars Chart-9). [1] The name Tharsis refers to a land mentioned in the Bible. It may be at the location of the old town of Tartessus at the mouth of Guadalquivir. [2]

Contents

The quadrangle covers the area from 90° to 135° west longitude and 0° to 30° north latitude on Mars and contains most of the Tharsis Rise. The plateau is about as high as Earth's Mount Everest and about as big in area as all of Europe. Tharsis contains a group of large volcanoes. Olympus Mons is the tallest. [3]

Within the quadrangle, the two largest impact craters are Poynting and Paros.

Volcanoes

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. [4] Pavonis Mons, the middle in a line of three volcanoes, sits at just about dead center on the equator. Mons is a term used for a large raised feature. Tholus is about the same, but smaller. A patera is flatter and like a volcano with a super large opening. Actually, a patera is formed when the top of a volcano collapses because its magma chamber is empty. Crater Lake Oregon was formed that way. Several volcanoes form a straight line in the Tharsis Uplift. Two major ones are in the Tharsus quadrangle: Ascraeus Mons and Pavonis Mons. It has been proposed that these are the result of plate motion which on Earth makes volcanic arc islands. [5] [6] [7] [8] [9]

Although Mars displays many volcanoes here and other places, there has been no evidence of recent volcanic activity, even at a very low level. Research, published in 2017, found no active release of volcanic gases during two successive Martian years. They looked for the outgassing of sulfur-bearing chemicals with spectrometers. [10]

Potential influence of volcanic emissions on climate

Some scientists maintain that Tharsis has had great influence on the climate of Mars. Volcanoes give off large amounts of gas when they erupt. The gases are usually water vapor and carbon dioxide. Some estimates put the amount of gas released to the atmosphere as enough to make the atmosphere thicker than the Earth's. In addition, the water released by the volcanoes could have been enough to cover all of Mars to a depth of 120 meters. The greenhouse effect of carbon dioxide raises the temperature of a planet by trapping heat in the form of infrared radiation. The volcanic eruptions on Tharsis could have made Mars more Earth-like in the past. Mars may have once had a much thicker and warmer atmosphere. Oceans and/or lakes may have been present. [3]

Fossae

Ulysses Fossae mound, as seen by HiRISE Ulysses Fossae mound.JPG
Ulysses Fossae mound, as seen by HiRISE

The Tharsis quadrangle is also home to large troughs (long narrow depressions) called fossae in the geographical language used for Mars. Fossae in this area are Ulysses Fossae, Olympica Fossae, Ceraunius Fossae, and Tractus Fossae. These troughs form when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano. Studies have shown that the volcanoes of Tharsis caused most of the major fossae on Mars. The stress that caused the fossae and other tectonic features is centered in Noctis Labyrinthus, at 4 S and 253 E. But the center has moved somewhat over time. [11] [12] Fossae/pit craters are common near volcanoes in the Tharsis and Elysium system of volcanoes. [13] A trough often has two breaks with a middle section moving down, leaving steep cliffs along the sides; such a trough is called a graben. [14] Studies have found that on Mars a fault may be as deep as 5 km, that is the break in the rock goes down to 5 km. Moreover, the crack or fault sometimes widens or dilates. This widening causes a void to form with a relatively high volume. When material slides into the void, a pit crater or a pit crater chain forms. Pit craters do not have rims or ejecta around them, like impact craters do. On Mars, individual pit craters can join to form chains or even to form troughs that are sometimes scalloped. [15] Other ideas have been suggested for the formation of fossae and pit craters. There is evidence that they are associated with dikes of magma. Magma might move along, under the surface, breaking the rock and, more importantly, melting ice. The resulting action would cause a crack to form at the surface. Pit craters are not common on Earth. Sinkholes, where the ground falls into a hole (sometimes in the middle of a town) resemble pit craters on Mars. However, on the Earth these holes are caused by limestone being dissolved thereby causing a void. [15] [16]

Knowledge of the locations and formation mechanisms of pit craters and fossae is important for the future colonization of Mars because they may be reservoirs of water. [17]

Glaciers

Some scientists see evidence that glaciers exist on many of the volcanoes in Tharsis, including Olympus Mons, Ascraeus Mons, and Pavonis Mons. [11] [18] [19] Ceraunius Tholus may have even had its glaciers melt to form some temporary lakes in the past. [20] [21] [22] [23] [24] [25] [26]

Ice sheets

Tharsis may have been the location for a giant ice sheet. [27] [28] [29] [30] [31] It would have been in the Late Hesperian time period. It may have melted quickly due to events like volcanism or impacts and it could have contributed to a northern ocean. [32] [33] [34] [35] Some researchers have suggested that lava flows covered the ice cap, thereby causing it to melt rather quickly. The water could have created the outflow channels around Tharsis. [36]

Dark slope streaks

Sulci Gordii Terraced Hills, as seen by HiRISE. Many dark slope streaks are visible. Sulci Gordii Terraced Hills.JPG
Sulci Gordii Terraced Hills, as seen by HiRISE. Many dark slope streaks are visible.

Some pictures below show dark streaks: on the slopes on large blocks just to the left of Tharsis Tholus, on Ceraunius Fossae, and on Olympica Fossae. Such streaks are common on Mars. They occur on steep slopes of craters, troughs, and valleys. The streaks are dark at first. They get lighter with age. [37] Sometimes they start in a tiny spot, then spread out and go for hundreds of meters. They have been seen to travel around obstacles, like boulders. [38] It is believed that they are avalanches of bright dust that expose a darker underlying layer. However, several ideas have been advanced to explain them. Some involve water or even the growth of organisms. [39] [40] The streaks appear in areas covered with dust. Much of the Martian surface is covered with dust. Fine dust settles out of the atmosphere covering everything. We know a lot about it because the solar panels of the Mars Rovers get covered with it, thus reducing the electrical energy. The power of the Rovers has been restored many times by the wind, in the form of dust devils, clearing the panels and thus boosting the power. [41] Dust storms are frequent, especially when the spring season begins in the southern hemisphere. At that time, Mars is 40% closer to the Sun. The orbit of Mars is much more elliptical then the Earth's. That is the difference between the farthest point from the Sun and the closest point to the Sun is very great for Mars, but only a slight amount for the Earth. Also, every few years, the entire planet is engulfed in global dust storms. When NASA's Mariner 9 craft arrived there, nothing could be seen through the dust storm. [42] [43] Other global dust storms have also been observed, since that time.

2764streaks.jpg
Image indicates crater cluster and curved lines formed by airblast from meteorites. Meteorites caused airblast which caused dust avalanches on steep slopes. Image is from HiRISE.
2764streaksclose.jpg
Close-up of previous image along light/dark boundary. Dark line in middle of image shows border between light and dark area of curved lines. Green arrows show high areas of ridges. Loose dust moved down steep slopes when it felt the airblast from meteorite strikes. Image is from HiRISE.

Research, published in January 2012 in Icarus, found that dark streaks were initiated by airblasts from meteorites traveling at supersonic speeds. The team of scientists was led by Kaylan Burleigh, an undergraduate at the University of Arizona. After counting some 65,000 dark streaks around the impact site of a group of five new craters, patterns emerged. The number of streaks was greatest closer to the impact site. So, the impact somehow probably caused the streaks. Also, the distribution of the streaks formed a pattern with two wings extending from the impact site. The curved wings resembled scimitars, curved knives. This pattern suggests that an interaction of airblasts from the group of meteorites shook dust loose enough to start dust avalanches that formed the many dark streaks. At first it was thought that the shaking of the ground from the impact caused the dust avalanches, but if that was the case the dark streaks would have been arranged symmetrically around the impacts, rather than being concentrated into curved shapes.

The crater cluster lies near the equator 510 miles) south of Olympus Mons, on a type of terrain called the Medusae Fossae formation. The formation is coated with dust and contains wind-carved ridges called yardangs. These yardangs have steep slopes thickly covered with dust, so when the sonic boom of the airblast arrived from the impacts dust started to move down the slope. Using photos from Mars Global Surveyor and HiRISE camera on NASA’s Mars Reconnaissance Orbiter, scientists have found about 20 new impacts each year on Mars. Because the spacecraft have been imaging Mars almost continuously for a span of 14 years, newer images with suspected recent craters can be compared to older images to determine when the craters were formed. Since the craters were spotted in a HiRISE image from February 2006, but were not present in a Mars Global Surveyor image taken in May 2004, the impact occurred in that time frame.

The largest crater in the cluster is about 22 meters (72 feet) in diameter with close to the area of a basketball court. As the meteorite traveled through the Martian atmosphere it probably broke up; hence a tight group of impact craters resulted. Dark slope streaks have been seen for some time, and many ideas have been advanced to explain them. [44] [45]


See also

Related Research Articles

<span class="mw-page-title-main">Tharsis</span> Volcanic plateau on Mars

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.

<span class="mw-page-title-main">Pavonis Mons</span> Martian volcano

Pavonis Mons 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 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 a space elevator location, especially in science fiction. It is also an ideal location for a Sky Ramp.

<span class="mw-page-title-main">Ascraeus Mons</span> Martian volcano

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.

In planetary nomenclature, a fossa is a long, narrow depression (trough) on the surface of an extraterrestrial body, such as a planet or moon. The term, which means "ditch" or "trench" in Latin, is not a geological term as such but a descriptor term used by the United States Geological Survey (USGS) and the International Astronomical Union (IAU) for topographic features whose geology or geomorphology is uncertain due to lack of data or knowledge of the exact processes that formed them. Fossae are believed to be the result of a number of geological processes, such as faulting or subsidence. Many fossae on Mars are probably graben.

<span class="mw-page-title-main">Alba Mons</span> Martian volcano

Alba Mons is a volcano located in the northern Tharsis region of the planet Mars. It is the biggest volcano on Mars in terms of surface area, with volcanic flow fields that extend for at least 1,350 km (840 mi) from its summit. Although the volcano has a span comparable to that of the United States, it reaches an elevation of only 6.8 km (22,000 ft) at its highest point. This is about one-third the height of Olympus Mons, the tallest volcano on the planet. The flanks of Alba Mons have very gentle slopes. The average slope along the volcano's northern 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.

<span class="mw-page-title-main">Elysium (volcanic province)</span> 2nd-largest volcanic region of Mars

Elysium, located in the Elysium and Cebrenia quadrangles, is the second largest volcanic region on Mars, after Tharsis. The region includes the volcanoes Hecates Tholus, Elysium Mons and Albor Tholus. The province is centered roughly on Elysium Mons at 24.7°N 150°E. Elysium Planitia is a broad plain to the south of Elysium, centered at 3.0°N 154.7°E. Another large volcano, Apollinaris Mons, lies south of Elysium Planitia and is not part of the province. Besides having large volcanoes, Elysium has several areas with long trenches, called fossa or fossae (plural) on Mars. They include the Cerberus Fossae, Elysium Fossae, Galaxias Fossae, Hephaestus Fossae, Hyblaeus Fossae, Stygis Fossae and Zephyrus Fossae.

<span class="mw-page-title-main">Volcanism on Mars</span>

Volcanic activity, or volcanism, has played a significant role in the geologic evolution of Mars. Scientists have known since the Mariner 9 mission in 1972 that volcanic features cover large portions of the Martian surface. These features include extensive lava flows, vast lava plains, and, such as Olympus Mons, the largest known volcanoes in the Solar System. Martian volcanic features range in age from Noachian to late Amazonian, indicating that the planet has been volcanically active throughout its history, and some speculate it probably still is so today. Both Mars and Earth are large, differentiated planets built from similar chondritic materials. Many of the same magmatic processes that occur on Earth also occurred on Mars, and both planets are similar enough compositionally that the same names can be applied to their igneous rocks.

<span class="mw-page-title-main">Medusae Fossae Formation</span> Large geological unit of uncertain origin on Mars

The Medusae Fossae Formation is a large geological formation of probable volcanic origin on the planet Mars. It is named for the Medusa of Greek mythology. "Fossae" is Latin for "trenches". The formation is a collection of soft, easily eroded deposits that extends discontinuously for more than 5,000 km along the equator of Mars. Its roughly-shaped regions extend from just south of Olympus Mons to Apollinaris Patera, with a smaller additional region closer to Gale Crater.

<span class="mw-page-title-main">Tharsis Tholus</span> Martian volcano

Tharsis Tholus is an intermediate-sized shield volcano located in the eastern Tharsis region of the planet Mars. The volcano was discovered by the Mariner 9 spacecraft in 1972 and originally given the informal name Volcano 7. In 1973, the International Astronomical Union (IAU) officially designated it Tharsis Tholus. In planetary geology, tholus is the term for a small domical mountain, usually a volcano.

<span class="mw-page-title-main">Cebrenia quadrangle</span> One of 30 quadrangle maps of Mars used by the US Geological Survey

The Cebrenia quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The quadrangle is located in the northeastern portion of Mars' eastern hemisphere and covers 120° to 180° east longitude and 30° to 65° north latitude. The quadrangle uses a Lambert conformal conic projection at a nominal scale of 1:5,000,000 (1:5M). The Cebrenia quadrangle is also referred to as MC-7. It includes part of Utopia Planitia and Arcadia Planitia. The southern and northern borders of the Cebrenia quadrangle are approximately 3,065 km (1,905 mi) and 1,500 km (930 mi) wide, respectively. The north to south distance is about 2,050 km (1,270 mi). The quadrangle covers an approximate area of 4.9 million square km, or a little over 3% of Mars' surface area.

<span class="mw-page-title-main">Diacria quadrangle</span> Map of Mars

The Diacria quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The quadrangle is located in the northwestern portion of Mars' western hemisphere and covers 180° to 240° east longitude and 30° to 65° north latitude. The quadrangle uses a Lambert conformal conic projection at a nominal scale of 1:5,000,000 (1:5M). The Diacria quadrangle is also referred to as MC-2. The Diacria quadrangle covers parts of Arcadia Planitia and Amazonis Planitia.

<span class="mw-page-title-main">Arcadia quadrangle</span> Map of Mars

The Arcadia quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The quadrangle is located in the north-central portion of Mars’ western hemisphere and covers 240° to 300° east longitude and 30° to 65° north latitude. The quadrangle uses a Lambert conformal conic projection at a nominal scale of 1:5,000,000 (1:5M). The Arcadia quadrangle is also referred to as MC-3. The name comes from a mountainous region in southern Greece. It was adopted by IAU, in 1958.

<span class="mw-page-title-main">Elysium quadrangle</span> One of 30 quadrangle maps of Mars used by the US Geological Survey

The Elysium quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Elysium quadrangle is also referred to as MC-15.

<span class="mw-page-title-main">Amazonis quadrangle</span> Map of Mars

The Amazonis quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Amazonis quadrangle is also referred to as MC-8.

<span class="mw-page-title-main">Phoenicis Lacus quadrangle</span> Map of Mars

The Phoenicis Lacus quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Phoenicis Lacus quadrangle is also referred to as MC-17. Parts of Daedalia Planum, Sinai Planum, and Solis Planum are found in this quadrangle. Phoenicis Lacus is named after the phoenix which according to myth burns itself up every 500 years and then is reborn.

<span class="mw-page-title-main">Ceraunius Fossae</span> Set of fractures in the northern Tharsis region of Mars

The Ceraunius Fossae are a set of fractures in the northern Tharsis region of Mars. They lie directly south of the large volcano Alba Mons and consist of numerous parallel faults and tension cracks that deform the ancient highland crust. In places, younger lava flows cover the fractured terrain, dividing it into several large patches or islands. They are found in the Tharsis quadrangle.

<span class="mw-page-title-main">Ceraunius Tholus</span> Martian volcano

Ceraunius Tholus is a volcano on Mars located in the Tharsis quadrangle at 24.25° north latitude and 262.75° east longitude, part of the Uranius group of volcanoes. It is 130 kilometres (81 mi) across, approximately 8,500 metres (27,887 ft) high and is named after a classical albedo feature name.

<span class="mw-page-title-main">Ulysses Fossae</span> Fossae on Mars

The Ulysses Fossae are a group of troughs in the Tharsis quadrangle of Mars at 10.06° north latitude and 123.07° west longitude. They were named after an albedo feature name. The area contains pitted cones called Ulysses Colles which were interpreted to be possible Martian equivalents to terrestrial cinder cones.

Mars may contain ores that would be very useful to 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.

<span class="mw-page-title-main">Rahe (crater)</span> Martian geographical feature

Rahe is a crater on the planet Mars in the Tharsis quadrangle, positioned at 25.05° north latitude and 262.52° east longitude, between the volcanoes Ceraunius Tholus and Uranius Tholus. It measures approximately 34 kilometers in diameter and was named after Jürgen Rahe, a German-American astronomer and NASA science program director.

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  36. ↑ J.P. Cassanelli, J.W. Head. 2019. Glaciovolcanism in the Tharsis volcanic province of Mars: Implications for regional geology and hydrology. Planet. Space Sci. pp. 45-69
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  38. ↑ updated, Space com Staff last (February 2, 2024). "Space pictures! See our space image of the day". Space.com.
  39. ↑ "SPACE.com -- Dark Streaks on Mars Suggest Running Water Still Present". Space.com . Archived from the original on 2008-04-27. Retrieved 2011-01-12.
  40. ↑ "Mars Coverage | Space". Space.com. May 20, 2024.
  41. ↑ "Mars Spirit Rover Gets Energy Boost From Cleaner Solar Panels". ScienceDaily. February 19, 2009. Retrieved January 11, 2011.
  42. ↑ Moore, Patrick (1990-06-02). Atlas of the Solar System. Crescent Books. ISBN   978-0-517-00192-9.
  43. ↑ Kieffer, Hugh H. (1992). Mars. Tucson: University of Arizona Press. pp.  &#91, page needed &#93, . ISBN   978-0-8165-1257-7.
  44. ↑ Burleigh, Kaylan J.; Melosh, Henry J.; Tornabene, Livio L.; Ivanov, Boris; McEwen, Alfred S.; Daubar, Ingrid J. (2012). "Impact air blast triggers dust avalanches on Mars". Icarus. 217 (1): 194–201. Bibcode:2012Icar..217..194B. doi:10.1016/j.icarus.2011.10.026.
  45. ↑ "Red Planet Report | What's new with Mars". redplanet.asu.edu.
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