Difference between revisions of "Sinus Sabaeus quadrangle"
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| − | The Sinus Sabaeus quadrangle contains a few very interesting craters. One contains a strange white rock in the center. Schiaparelli is a large, easily located crater on the equator. There are several neat exposures of layers in | + | The Sinus Sabaeus quadrangle contains a few very interesting craters. One contains a strange white rock in the center. Another crater, Schiaparelli, is a large, easily located crater on the equator. There are several neat exposures of layers in this quadrangle. Most of the region contains heavily cratered highlands. |
In this article, some of the best pictures from a number of spacecraft will show what the landscape looks like in this region. The origins and significance of all features will be explained as they are currently understood. | In this article, some of the best pictures from a number of spacecraft will show what the landscape looks like in this region. The origins and significance of all features will be explained as they are currently understood. | ||
| − | The Sinus Sabaeus quadrangle is one of a series of 30 quadrangle maps of Mars | + | The Sinus Sabaeus quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS). It is also referred to as MC-20 (Mars Chart-20).<ref>Davies, M.E.; Batson, R.M.; Wu, S.S.C. “Geodesy and Cartography” in Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W.; Matthews, M.S., Eds. ''Mars.'' University of Arizona Press: Tucson, 1992.</ref> |
The Sinus Sabaeus quadrangle covers the area from and 0° to 30° degrees south latitude and 315° to 360° west longitude (45-0 E). The Sinus Sabaeus quadrangle contains parts of regions that have classical names: Noachis Terra and Terra Sabaea. | The Sinus Sabaeus quadrangle covers the area from and 0° to 30° degrees south latitude and 315° to 360° west longitude (45-0 E). The Sinus Sabaeus quadrangle contains parts of regions that have classical names: Noachis Terra and Terra Sabaea. | ||
The name comes from an incense-rich location south of the Arabian peninsula (the Gulf of Aden).<ref>Blunck, J. 1982. Mars and its Satellites. Exposition Press. Smithtown, N.Y.</ref> | The name comes from an incense-rich location south of the Arabian peninsula (the Gulf of Aden).<ref>Blunck, J. 1982. Mars and its Satellites. Exposition Press. Smithtown, N.Y.</ref> | ||
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Wislicenus Crater and the Schiaparelli basin crater contain layers, also called strata. Many places on Mars show rocks arranged in layers.<ref>Grotzinger, J. and R. Milliken (eds.) 2012. Sedimentary Geology of Mars. SEPM</ref> Sometimes the layers are of different colors. Light-toned rocks on Mars have been associated with hydrated minerals like sulfates. The Mars Rover Opportunity examined such layers close-up with several instruments and detected clay (also called phyllosilicates if you like big words) and found out that light-toned rocks often contain hydrated minerals. Both need water to form. These minerals were mapped with instruments on orbiting spacecraft, but the rover on the ground supplied ground truth. Scientists are excited about finding hydrated minerals such as sulfates and clays on Mars because they are usually formed in the presence of water.<ref>http://themis.asu.edu/features/nilosyrtis</ref> Places that contain clays and/or other hydrated minerals would be good places to look for evidence of life.<ref>http://hirise.lpl.arizona.edu/PSP_004046_2080</ref> In plain words, if we see light-toned materials, we suspect water once existed there. | Wislicenus Crater and the Schiaparelli basin crater contain layers, also called strata. Many places on Mars show rocks arranged in layers.<ref>Grotzinger, J. and R. Milliken (eds.) 2012. Sedimentary Geology of Mars. SEPM</ref> Sometimes the layers are of different colors. Light-toned rocks on Mars have been associated with hydrated minerals like sulfates. The Mars Rover Opportunity examined such layers close-up with several instruments and detected clay (also called phyllosilicates if you like big words) and found out that light-toned rocks often contain hydrated minerals. Both need water to form. These minerals were mapped with instruments on orbiting spacecraft, but the rover on the ground supplied ground truth. Scientists are excited about finding hydrated minerals such as sulfates and clays on Mars because they are usually formed in the presence of water.<ref>http://themis.asu.edu/features/nilosyrtis</ref> Places that contain clays and/or other hydrated minerals would be good places to look for evidence of life.<ref>http://hirise.lpl.arizona.edu/PSP_004046_2080</ref> In plain words, if we see light-toned materials, we suspect water once existed there. | ||
| + | |||
Rock can form layers in a variety of ways. Volcanoes, wind, or water can produce layers.<ref>http://hirise.lpl.arizona.edu?PSP_008437_1750</ref> Layers can be hardened by the action of groundwater. Martian ground water probably moved hundreds of kilometers, and in the process it dissolved many minerals from the rock it passed through. When ground water surfaces in low areas containing sediments, water evaporates in the thin atmosphere and leaves behind minerals as deposits and/or cementing agents. Consequently, layers of dust could not later easily erode away since they were cemented together. On Earth, mineral-rich waters often evaporate forming large deposits of various types of salts and other minerals. Sometimes water flows through Earth's aquifers, and then evaporates at the surface just as is hypothesized for Mars. One location this occurs on Earth is the Great Artesian Basin of Australia.<ref>Habermehl, M. A. (1980) The Great Artesian Basin, Australia. J. Austr. Geol. Geophys. 5, 9–38.</ref> On Earth the hardness of many sedimentary rocks, like sandstone, is largely due to the cement that was put in place as water passed through. | Rock can form layers in a variety of ways. Volcanoes, wind, or water can produce layers.<ref>http://hirise.lpl.arizona.edu?PSP_008437_1750</ref> Layers can be hardened by the action of groundwater. Martian ground water probably moved hundreds of kilometers, and in the process it dissolved many minerals from the rock it passed through. When ground water surfaces in low areas containing sediments, water evaporates in the thin atmosphere and leaves behind minerals as deposits and/or cementing agents. Consequently, layers of dust could not later easily erode away since they were cemented together. On Earth, mineral-rich waters often evaporate forming large deposits of various types of salts and other minerals. Sometimes water flows through Earth's aquifers, and then evaporates at the surface just as is hypothesized for Mars. One location this occurs on Earth is the Great Artesian Basin of Australia.<ref>Habermehl, M. A. (1980) The Great Artesian Basin, Australia. J. Austr. Geol. Geophys. 5, 9–38.</ref> On Earth the hardness of many sedimentary rocks, like sandstone, is largely due to the cement that was put in place as water passed through. | ||
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Image:Bouguercraterhirise.jpg|Close up of layers in eroded deposits on the floor of Bouguer Crater, as seen by HiRISE. This image is in a different part of the crater than the previous image. | Image:Bouguercraterhirise.jpg|Close up of layers in eroded deposits on the floor of Bouguer Crater, as seen by HiRISE. This image is in a different part of the crater than the previous image. | ||
| − | Image:Layers in Monument Valley.jpg|Layers in Monument Valley. These are accepted as being formed, at least in part, | + | Image:Layers in Monument Valley.jpg|Layers in Monument Valley. These are accepted as being formed, at least in part, with the aid of water. Since Mars contains similar layers, water remains as a major cause of layering. |
Image:26876whitelayers.jpg|White layers that may be related to the white material in Pollack Crater, as seen by HiRISE under [[HiWish program]]. | Image:26876whitelayers.jpg|White layers that may be related to the white material in Pollack Crater, as seen by HiRISE under [[HiWish program]]. | ||
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Layers in crater found within the Schiaparelli Crater basin as seen by Mars Global Surveyor | Layers in crater found within the Schiaparelli Crater basin as seen by Mars Global Surveyor | ||
| − | Schiaparelli is an impact crater located near Mars's equator. It is 461 km in diameter and located at latitude 3° south and longitude 344° W. Some places within Schiaparelli show many layers that may have formed by the wind, volcanoes, or deposition under water. Some are quite beautiful as shown in the pictures below. People often seek to travel to our national parks like the Grand Canyon to see layers like the ones in Schiaparelli. | + | Schiaparelli is an impact crater located near Mars's equator. It is 461 km in diameter and located at latitude 3° south and longitude 344° W. Some places within Schiaparelli show many layers that may have formed by the wind, volcanoes, or deposition under water. Some are quite beautiful as shown in the pictures above and below. People often seek to travel to our national parks like the Grand Canyon to see layers like the ones in Schiaparelli. |
<gallery class="center" widths="380px" heights="360px"> | <gallery class="center" widths="380px" heights="360px"> | ||
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| + | Image:ESP 028511rings.jpg|Circular structures on floor of Schiaparelli Crater | ||
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| + | 46814 1785layeredmound.jpg|Layered mound in Schiaparelli Crater | ||
| − | 46814 | + | File: 46814 1785layeredmound2.jpg|Layers in Schiaparelli Crater |
| − | + | 46814 1785layeresleft.jpg|Layers in Schiaparelli Crater | |
| − | |||
| + | 46814 1785layerscloseleftbottom.jpg|Close view of layers in Schiaparelli Crater, as seen by HiRISE under[[ HiWish ]] Dark sand is visible on some layers. | ||
| − | + | ESP 046814 1785layersclosecolor.jpg|Close, color view of layers in Schiaparelli Crater Dark sand is visible on some layers. | |
| − | ESP 046814 1785layersclosecolor.jpg|Close, color view of layers in Schiaparelli Crater | ||
</gallery> | </gallery> | ||
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== Other Craters == | == Other Craters == | ||
| − | When a comet or asteroid collides at a high rate of speed with the surface of Mars, it creates a primary impact crater. The primary impact may also eject significant numbers of rocks which eventually fall back to make secondary craters.<ref>http://hirise.lpl.arizona.edu/science_themes/impact.php</ref> Secondary craters may be arranged in clusters. | + | When a comet or asteroid collides at a high rate of speed with the surface of Mars, it creates a primary impact crater. The primary impact may also eject significant numbers of rocks which eventually fall back to make secondary craters.<ref>http://hirise.lpl.arizona.edu/science_themes/impact.php</ref> Secondary craters may be arranged in clusters. If secondary craters formed from a single, large, nearby impact, then they would have formed at roughly the same instant in time and be of the same age--which is how they appear below in the image of Denning Crater. |
<gallery class="center" widths="380px" heights="360px"> | <gallery class="center" widths="380px" heights="360px"> | ||
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| + | Wikibakhuysen.jpg|Bakhuysen Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Channels are visible on the north (top) and south (bottom) rims of crater. | ||
| + | </gallery> | ||
| + | [[File:Wikibakhuysenchannels.jpg |600pxr|Channels on south rim of Bakhuysen Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image of Bakhuysen Crater.]] | ||
| + | Channels on south rim of Bakhuysen Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image of Bakhuysen Crater. | ||
| + | <gallery class="center" widths="380px" heights="360px"> | ||
| + | File:75431 1665ejecta2.jpg|Crater with colorful ejecta, as seen by HiRISE under the HiWish program The ejecta represents samples of material from underground. Craters allow us to study underlying material. | ||
| − | + | File:75431 1665ejecta3.jpg|Crater with colorful ejecta, as seen by HiRISE The ejecta represents samples of material from underground. Craters allow us to study underlying material. | |
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| − | . | ||
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</gallery> | </gallery> | ||
== White rock in Pollack crater == | == White rock in Pollack crater == | ||
| − | Within | + | Within this quadrangle is Pollack crater, which has light-toned rock deposits. Mars has an old surface compared to Earth. While much of Earth's land surface is just a few hundred million years old, large areas of Mars are billions of years old. Some surface areas have been formed, eroded away, and then covered over with new layers of rocks. The [[Mariner 9]] spacecraft in the 1970s photographed a feature that was called "White Rock." Newer images revealed that the rock is not really white, but that the area close by is so dark that the white rock looks really white.<ref> Grotzinger, J. and R. Milliken (eds.) 2012. Sedimentary Geology of Mars. SEPM</ref> It was thought that this feature could have been a salt deposit, but information from the instruments on [[Mars Global Surveyor]] demonstrated rather that it was probably volcanic ash or dust. Today, it is believed that White Rock represents an old rock layer that once filled the whole crater that it's in, but today the whitish rock has since been mostly eroded away. The picture below shows white rock with a spot of the same rock some distance from the main deposit, so it is thought that the white material once covered a far larger area.<ref>http://space.com/scienceastronomy/solarsystem/mars_daily_020419.html</ref> |
<gallery class="center" widths="380px" heights="360px"> | <gallery class="center" widths="380px" heights="360px"> | ||
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==Channels in Sinus Sabaeus quadrangle== | ==Channels in Sinus Sabaeus quadrangle== | ||
| − | There is enormous evidence that water once flowed in river valleys on Mars.<ref>Baker, V., et al. 2015. Fluvial geomorphology on Earth-like planetary surfaces: a review. Geomorphology. 245, 149–182.</ref> <ref>Carr, M. 1996. in Water on Mars. Oxford Univ. Press.</ref> Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the [[Mariner 9]] orbiter.<ref>Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX</ref> <ref>Baker, V., R. Strom, R., V. Gulick, J. Kargel, G. Komatsu, V. Kale. 1991. Ancient oceans, ice sheets and the hydrological cycle on Mars. Nature 352, 589–594.</ref> <ref>Carr, M. 1979. Formation of Martian flood features by release of water from confined aquifers. J. Geophys. Res. 84, 2995–300.</ref> <ref>Komar, P. 1979. Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth. Icarus 37, 156–181.</ref> Indeed, a study published in June 2017, calculated that the volume of water needed to carve all the channels on Mars was even larger than the proposed ocean that the planet may have had. Water was probably recycled many times from the ocean to rainfall around Mars.<ref>http://spaceref.com/mars/how-much-water-was-needed-to-carve-valleys-on-mars.html</ref> <ref>Luo, W., et al. 2017. New Martian valley network volume estimate consistent with ancient ocean and warm and wet climate. Nature Communications 8. Article number: 15766 (2017). doi:10.1038/ncomms15766</ref> | + | There is enormous evidence that water once flowed in river valleys on Mars.<ref>Baker, V., et al. 2015. Fluvial geomorphology on Earth-like planetary surfaces: a review. Geomorphology. 245, 149–182.</ref> <ref>Carr, M. 1996. in Water on Mars. Oxford Univ. Press.</ref> Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the [[Mariner 9]] orbiter.<ref>Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX</ref> <ref>Baker, V., R. Strom, R., V. Gulick, J. Kargel, G. Komatsu, V. Kale. 1991. Ancient oceans, ice sheets and the hydrological cycle on Mars. Nature 352, 589–594.</ref> <ref>Carr, M. 1979. Formation of Martian flood features by release of water from confined aquifers. J. Geophys. Res. 84, 2995–300.</ref> <ref>Komar, P. 1979. Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth. Icarus 37, 156–181.</ref> As Mars has been studied in the decades since Mariner 9, more and more river-like forms have been seen. Indeed, a study published in June 2017, calculated that the volume of water needed to carve all the channels on Mars was even larger than the proposed ocean that the planet may have had. Water was probably recycled many times from the ocean to rainfall around Mars.<ref>http://spaceref.com/mars/how-much-water-was-needed-to-carve-valleys-on-mars.html</ref> <ref>Luo, W., et al. 2017. New Martian valley network volume estimate consistent with ancient ocean and warm and wet climate. Nature Communications 8. Article number: 15766 (2017). doi:10.1038/ncomms15766</ref> |
| + | |||
| + | Many crater contained lakes. Some craters in the Sinus Sabaeus quadrangle are believed to have formed from the melting of glaciers on their rims. Inverted streams are found on the floors of some craters. Water from glaciers carried debris in channels and consequently that debris was left behind after the surrounding ground eroded.<ref>Boatwright, B., et al. 2021. INVERTED FLUVIAL CHANNELS IN TERRA SABAEA, MARS: GEOMORPHIC EVIDENCE FOR | ||
| + | PROGLACIAL LAKES AND WIDESPREAD HIGHLANDS GLACIATION IN THE LATE NOACHIAN. 52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548). 1641.pdf</ref> <ref>https://www.brown.edu/news/2021-03-30/crater-lake?fbclid=IwAR0QGkqpUazmc4qCTgDVzGdYuprxiuqQK0hGkfraGR0hg8z63DmaT_bO4FQ</ref> | ||
| + | |||
<gallery class="center" widths="190px" heights="180px" > | <gallery class="center" widths="190px" heights="180px" > | ||
| − | ESP 041974 1740channel.jpg|Winding channel | + | ESP 041974 1740channel.jpg|Winding channel |
| − | ESP 045813 1510channels.jpg|Channels | + | ESP 045813 1510channels.jpg|Channels |
| − | ESP 051192 1555channel.jpg|Channels, as seen by HiRISE under HiWish program | + | ESP 051192 1555channel.jpg|Channels, as seen by HiRISE under [[HiWish program]] |
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<gallery class="center" widths="380px" heights="360px"> | <gallery class="center" widths="380px" heights="360px"> | ||
| − | File:ESP 057415 1740ridge.jpg|This straight ridge may be a dike that has been exposed by erosion. It was initially formed by magma moving under the surface along weak spots. | + | File:ESP 057415 1740ridge.jpg|This straight ridge may be a dike that has been exposed by erosion. It was initially formed by magma moving under the surface along weak spots. |
| − | ESP 047368 1665ridge.jpg| | + | ESP 047368 1665ridge.jpg|Another long, straight ridge may be a dike that has been exposed by erosion. It was initially formed by magma moving under the surface. The picture was taken with HiRISE under the HiWish program. |
</gallery> | </gallery> | ||
== Dunes == | == Dunes == | ||
| + | |||
| + | Dunes of various shapes are common on Mars, especially on the floors of craters. Sand gets into craters and then the winds are not strong enough to get it over the rim. Although Mars can have wind with a high velocity, the wind lacks power since the air is so thin--only 1 % of the Earth. | ||
<gallery class="center" widths="380px" heights="360px"> | <gallery class="center" widths="380px" heights="360px"> | ||
| + | File:ESP 054976 1685dunes.jpg|Dunes, as seen with HiRISE under the HiWish program. | ||
| + | </gallery> | ||
| + | |||
| + | Dunes of various shapes are common on Mars, especially on the floors of craters. Sand gets into craters and then the winds are not strong enough to get it over the rim. Although Mars can have wind with a high velocity, the wind lacks power since the air is so thin--only 1 % of the Earth. ' | ||
| + | |||
| + | <gallery class="center" widths="380px" heights="360px"> | ||
| + | File:ESP 082974 1685ridge and star shaped dunes 01.jpg|Wide view of crater showing ridges and varioujs shaped sand dunes on floor. | ||
| + | |||
| + | File:ESP 082974 1685ridge and star shaped dunes 02.jpg|Close view of various shaped dunes Picture is about 1 km across. | ||
| + | File:ESP 082974 1685 star shaped dunes 03.jpg|Close view of various shaped dunes Picture is about 1 km across. Some dunes would be called star dunes. | ||
| + | File:ESP 082974 1685ridge and star shaped dunes 04.jpg|Close view of various shaped dunes Picture is about 1 km across. | ||
| + | File:ESP 082974 1685 star shaped dunes 03.jpg|Close view of various shaped dunes Picture is about 1 km across. Some dunes would be called star dunes. | ||
| + | File:ESP 082974 1685star shaped dunes 05.jpg|Close view of various shaped dunes Picture is about 1 km across. | ||
| + | </gallery> | ||
| + | ==Other scenes in Sinus Sabaeus quadrangle== | ||
| − | File:ESP | + | <gallery class="center" widths="380px" heights="360px"> |
| + | |||
| + | File:ESP 080784 2035mesaboulders 01.jpg|Wide view of mesas, as seen by HiRISE under HiWish program | ||
| + | File:Mesa with possible tracks of boulders.jpg | ||
| + | File:Boulders and cap rock of a mesa.jpg|Close view of mesa, as seen by HiRISE House-sized boulders are present in abundance. This image was named HiRISE picture of the day for November 14, 2023. | ||
| + | File:Cap rock and layers of a mesa.jpg|Close view of cap rock, as seen by HiRISE The cap rock overhangs some layers. The cap rock was more resistant to erosion, so it formed an overhang. | ||
</gallery> | </gallery> | ||
Latest revision as of 05:55, 9 October 2024
| MC-20 | Sinus Sabaeus | 0–30° S | 0–45° E | Quadrangles | Atlas |
The Sinus Sabaeus quadrangle contains a few very interesting craters. One contains a strange white rock in the center. Another crater, Schiaparelli, is a large, easily located crater on the equator. There are several neat exposures of layers in this quadrangle. Most of the region contains heavily cratered highlands. In this article, some of the best pictures from a number of spacecraft will show what the landscape looks like in this region. The origins and significance of all features will be explained as they are currently understood. The Sinus Sabaeus quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS). It is also referred to as MC-20 (Mars Chart-20).[1] The Sinus Sabaeus quadrangle covers the area from and 0° to 30° degrees south latitude and 315° to 360° west longitude (45-0 E). The Sinus Sabaeus quadrangle contains parts of regions that have classical names: Noachis Terra and Terra Sabaea. The name comes from an incense-rich location south of the Arabian peninsula (the Gulf of Aden).[2]
Contents
Layers
Wislicenus Crater and the Schiaparelli basin crater contain layers, also called strata. Many places on Mars show rocks arranged in layers.[3] Sometimes the layers are of different colors. Light-toned rocks on Mars have been associated with hydrated minerals like sulfates. The Mars Rover Opportunity examined such layers close-up with several instruments and detected clay (also called phyllosilicates if you like big words) and found out that light-toned rocks often contain hydrated minerals. Both need water to form. These minerals were mapped with instruments on orbiting spacecraft, but the rover on the ground supplied ground truth. Scientists are excited about finding hydrated minerals such as sulfates and clays on Mars because they are usually formed in the presence of water.[4] Places that contain clays and/or other hydrated minerals would be good places to look for evidence of life.[5] In plain words, if we see light-toned materials, we suspect water once existed there.
Rock can form layers in a variety of ways. Volcanoes, wind, or water can produce layers.[6] Layers can be hardened by the action of groundwater. Martian ground water probably moved hundreds of kilometers, and in the process it dissolved many minerals from the rock it passed through. When ground water surfaces in low areas containing sediments, water evaporates in the thin atmosphere and leaves behind minerals as deposits and/or cementing agents. Consequently, layers of dust could not later easily erode away since they were cemented together. On Earth, mineral-rich waters often evaporate forming large deposits of various types of salts and other minerals. Sometimes water flows through Earth's aquifers, and then evaporates at the surface just as is hypothesized for Mars. One location this occurs on Earth is the Great Artesian Basin of Australia.[7] On Earth the hardness of many sedimentary rocks, like sandstone, is largely due to the cement that was put in place as water passed through.
Wislicenus Crater Floor, as seen by HiRISE. Erosion on floor has made layers visible.
Bouguer Crater) as seen by CTX. Crater rim is at top. Small craters are on floor of the crater.
Close up of layers in eroded deposits on the floor of Bouguer Crater, as seen by HiRISE. This image is in a different part of the crater than the previous image.
Layers in Monument Valley. These are accepted as being formed, at least in part, with the aid of water. Since Mars contains similar layers, water remains as a major cause of layering.
White layers that may be related to the white material in Pollack Crater, as seen by HiRISE under HiWish program.
Schiaparelli Crater
Layers in crater found within the Schiaparelli Crater basin as seen by Mars Global Surveyor
Schiaparelli is an impact crater located near Mars's equator. It is 461 km in diameter and located at latitude 3° south and longitude 344° W. Some places within Schiaparelli show many layers that may have formed by the wind, volcanoes, or deposition under water. Some are quite beautiful as shown in the pictures above and below. People often seek to travel to our national parks like the Grand Canyon to see layers like the ones in Schiaparelli.
MOLA map of area around Schiaparelli Crater
Circular structures on floor of Schiaparelli Crater
Layered mound in Schiaparelli Crater
Layers in Schiaparelli Crater
Layers in Schiaparelli Crater
Close view of layers in Schiaparelli Crater, as seen by HiRISE underHiWish Dark sand is visible on some layers.
Close, color view of layers in Schiaparelli Crater Dark sand is visible on some layers.
Close view of layers and rough terrain in Northwestern Schiaparelli Crater, as seen by HiRISE under HiWish program
Other Craters
When a comet or asteroid collides at a high rate of speed with the surface of Mars, it creates a primary impact crater. The primary impact may also eject significant numbers of rocks which eventually fall back to make secondary craters.[8] Secondary craters may be arranged in clusters. If secondary craters formed from a single, large, nearby impact, then they would have formed at roughly the same instant in time and be of the same age--which is how they appear below in the image of Denning Crater.
Recent small crater on floor of Denning Crater, as seen by HiRISE. Arrow shows group of secondary craters from ejecta falling down.
Group of secondary craters, as seen by HiRISE under HiWish program
Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. Sometimes craters expose layers that were buried. Rocks from deep underground are tossed onto the surface. Hence, craters can show us what lies deep under the surface.
Bakhuysen Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Channels are visible on the north (top) and south (bottom) rims of crater.
Channels on south rim of Bakhuysen Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image of Bakhuysen Crater.
Crater with colorful ejecta, as seen by HiRISE under the HiWish program The ejecta represents samples of material from underground. Craters allow us to study underlying material.
Crater with colorful ejecta, as seen by HiRISE The ejecta represents samples of material from underground. Craters allow us to study underlying material.
White rock in Pollack crater
Within this quadrangle is Pollack crater, which has light-toned rock deposits. Mars has an old surface compared to Earth. While much of Earth's land surface is just a few hundred million years old, large areas of Mars are billions of years old. Some surface areas have been formed, eroded away, and then covered over with new layers of rocks. The Mariner 9 spacecraft in the 1970s photographed a feature that was called "White Rock." Newer images revealed that the rock is not really white, but that the area close by is so dark that the white rock looks really white.[9] It was thought that this feature could have been a salt deposit, but information from the instruments on Mars Global Surveyor demonstrated rather that it was probably volcanic ash or dust. Today, it is believed that White Rock represents an old rock layer that once filled the whole crater that it's in, but today the whitish rock has since been mostly eroded away. The picture below shows white rock with a spot of the same rock some distance from the main deposit, so it is thought that the white material once covered a far larger area.[10]
White Rock in Pollack Crater as seen by HiRISE.
Enlargement of White Rock in Pollack Crater, as seen by HiRISE.
Whiterock on crater floor may be what's left of a much larger deposit. Arrow shows that the deposit once reached much farther. Picture taken by THEMIS.
Channels in Sinus Sabaeus quadrangle
There is enormous evidence that water once flowed in river valleys on Mars.[11] [12] Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the Mariner 9 orbiter.[13] [14] [15] [16] As Mars has been studied in the decades since Mariner 9, more and more river-like forms have been seen. Indeed, a study published in June 2017, calculated that the volume of water needed to carve all the channels on Mars was even larger than the proposed ocean that the planet may have had. Water was probably recycled many times from the ocean to rainfall around Mars.[17] [18]
Many crater contained lakes. Some craters in the Sinus Sabaeus quadrangle are believed to have formed from the melting of glaciers on their rims. Inverted streams are found on the floors of some craters. Water from glaciers carried debris in channels and consequently that debris was left behind after the surrounding ground eroded.[19] [20]
Winding channel
Channels
Channels, as seen by HiRISE under HiWish program
Ridges
This straight ridge may be a dike that has been exposed by erosion. It was initially formed by magma moving under the surface along weak spots.
Another long, straight ridge may be a dike that has been exposed by erosion. It was initially formed by magma moving under the surface. The picture was taken with HiRISE under the HiWish program.
Dunes
Dunes of various shapes are common on Mars, especially on the floors of craters. Sand gets into craters and then the winds are not strong enough to get it over the rim. Although Mars can have wind with a high velocity, the wind lacks power since the air is so thin--only 1 % of the Earth.
Dunes, as seen with HiRISE under the HiWish program.
Dunes of various shapes are common on Mars, especially on the floors of craters. Sand gets into craters and then the winds are not strong enough to get it over the rim. Although Mars can have wind with a high velocity, the wind lacks power since the air is so thin--only 1 % of the Earth. '
Wide view of crater showing ridges and varioujs shaped sand dunes on floor.
Close view of various shaped dunes Picture is about 1 km across.
Close view of various shaped dunes Picture is about 1 km across. Some dunes would be called star dunes.
Close view of various shaped dunes Picture is about 1 km across.
Close view of various shaped dunes Picture is about 1 km across. Some dunes would be called star dunes.
Close view of various shaped dunes Picture is about 1 km across.
Other scenes in Sinus Sabaeus quadrangle
Wide view of mesas, as seen by HiRISE under HiWish program
Close view of mesa, as seen by HiRISE House-sized boulders are present in abundance. This image was named HiRISE picture of the day for November 14, 2023.
Close view of cap rock, as seen by HiRISE The cap rock overhangs some layers. The cap rock was more resistant to erosion, so it formed an overhang.
See also
- High Resolution Imaging Science Experiment (HiRISE)
- HiWish program
- Layers on Mars
- Mars Global Surveyor
- Rivers on Mars
References
Further reading
- Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.
External links
- ↑ Davies, M.E.; Batson, R.M.; Wu, S.S.C. “Geodesy and Cartography” in Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W.; Matthews, M.S., Eds. Mars. University of Arizona Press: Tucson, 1992.
- ↑ Blunck, J. 1982. Mars and its Satellites. Exposition Press. Smithtown, N.Y.
- ↑ Grotzinger, J. and R. Milliken (eds.) 2012. Sedimentary Geology of Mars. SEPM
- ↑ http://themis.asu.edu/features/nilosyrtis
- ↑ http://hirise.lpl.arizona.edu/PSP_004046_2080
- ↑ http://hirise.lpl.arizona.edu?PSP_008437_1750
- ↑ Habermehl, M. A. (1980) The Great Artesian Basin, Australia. J. Austr. Geol. Geophys. 5, 9–38.
- ↑ http://hirise.lpl.arizona.edu/science_themes/impact.php
- ↑ Grotzinger, J. and R. Milliken (eds.) 2012. Sedimentary Geology of Mars. SEPM
- ↑ http://space.com/scienceastronomy/solarsystem/mars_daily_020419.html
- ↑ Baker, V., et al. 2015. Fluvial geomorphology on Earth-like planetary surfaces: a review. Geomorphology. 245, 149–182.
- ↑ Carr, M. 1996. in Water on Mars. Oxford Univ. Press.
- ↑ Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX
- ↑ Baker, V., R. Strom, R., V. Gulick, J. Kargel, G. Komatsu, V. Kale. 1991. Ancient oceans, ice sheets and the hydrological cycle on Mars. Nature 352, 589–594.
- ↑ Carr, M. 1979. Formation of Martian flood features by release of water from confined aquifers. J. Geophys. Res. 84, 2995–300.
- ↑ Komar, P. 1979. Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth. Icarus 37, 156–181.
- ↑ http://spaceref.com/mars/how-much-water-was-needed-to-carve-valleys-on-mars.html
- ↑ Luo, W., et al. 2017. New Martian valley network volume estimate consistent with ancient ocean and warm and wet climate. Nature Communications 8. Article number: 15766 (2017). doi:10.1038/ncomms15766
- ↑ Boatwright, B., et al. 2021. INVERTED FLUVIAL CHANNELS IN TERRA SABAEA, MARS: GEOMORPHIC EVIDENCE FOR PROGLACIAL LAKES AND WIDESPREAD HIGHLANDS GLACIATION IN THE LATE NOACHIAN. 52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548). 1641.pdf
- ↑ https://www.brown.edu/news/2021-03-30/crater-lake?fbclid=IwAR0QGkqpUazmc4qCTgDVzGdYuprxiuqQK0hGkfraGR0hg8z63DmaT_bO4FQ
