Difference between revisions of "Amenthes quadrangle"
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| − | The Amenthes quadrangle contains features with names like Isidis, Amenthes Fossae, Libya Montes, and Escalente Crater. Nearly all the names of Martian locations are from old writings like the Bible and Homer. Early astronomers gave names to things they saw on Mars. Things were given names and then other names, over and over. Finally the astronomer Giovanni Schiaparelli, after making drawings when Mars was exceptionally close in 1887, assigned the names still use today, over a hundred years later.<ref> Macdonald, T. 1971. The origins of Martian Nomenclature. Icarus: 15, 233-240.</ref> <ref> Glasstone, S. 1968. The Book of Mars. NASA. Washington, D.C</ref> Giovanni Schiaparelli is called the Father of Mars—at one point he knew more about Mars than any other living person. The name Amenthes is the Egyptian word for the place where the souls of the dead go.<ref>Blunck, J. 1982. Mars and its Satellites. Exposition Press. Smithtown, N.Y.</ref> | + | The Amenthes quadrangle contains features with names like [[Isidis Planitia|Isidis]], Amenthes Fossae, Libya Montes, and Escalente Crater. Nearly all the names of Martian locations are from old writings like the Bible and Homer. Early astronomers gave names to things they saw on Mars. Things were given names and then other names, over and over. Finally the astronomer Giovanni Schiaparelli, after making drawings when Mars was exceptionally close in 1887, assigned the names still in use today, over a hundred years later.<ref>Macdonald, T. 1971. The origins of Martian Nomenclature. Icarus: 15, 233-240.</ref> <ref>Glasstone, S. 1968. The Book of Mars. NASA. Washington, D.C</ref> Giovanni Schiaparelli is called the Father of Mars—at one point he knew more about Mars than any other living person. The name Amenthes is the Egyptian word for the place where the souls of the dead go.<ref>Blunck, J. 1982. Mars and its Satellites. Exposition Press. Smithtown, N.Y.</ref> |
| + | |||
| + | 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. | ||
| + | |||
==Location== | ==Location== | ||
| − | The Amenthes | + | |
| + | The Amenthes quadrangle covers the area from 0° to 30° north latitude and 225° to 270° west longitude (135-90 E). Amenthes quadrangle contains parts of Utopia Planitia, Isidis Planitia, Terra Cimmeria, and Tyrrhena Terra. There are different ways of telling positions on Mars. One can just give coordinates. One can use one of the maps that have been produced form old drawings dating back to Schiaparelli--this is usually done. Here we are going by a system where the surface of Mars is divided into 30 regions, called quadrangles. Nearly all of the quadrangles use the classical names. | ||
So, Amenthes quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS). The Amenthes quadrangle is also referred to as MC-14 (Mars Chart-14).<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> | So, Amenthes quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS). The Amenthes quadrangle is also referred to as MC-14 (Mars Chart-14).<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> | ||
| − | ==Significant facts == | + | ==Significant facts== |
| + | |||
The Amenthes quadrangle contains several features commonplace on Mars. It has dark slope streaks, troughs (fossae), and river valleys (Vallis {word used in planetary geology}) in this quadrangle. | The Amenthes quadrangle contains several features commonplace on Mars. It has dark slope streaks, troughs (fossae), and river valleys (Vallis {word used in planetary geology}) in this quadrangle. | ||
This quadrangle contains the Isidis basin, a location where magnesium carbonate was found by Mars Reconnaissance Orbiter. This mineral indicates that water was present and that it was not acidic. This fact increases the chances of life here in the past. Although some organisms can live in an acid environment, most living things do not thrive in an acid environment. | This quadrangle contains the Isidis basin, a location where magnesium carbonate was found by Mars Reconnaissance Orbiter. This mineral indicates that water was present and that it was not acidic. This fact increases the chances of life here in the past. Although some organisms can live in an acid environment, most living things do not thrive in an acid environment. | ||
| − | The [[Beagle 2]] lander was about to land in the quadrangle, particularly in the eastern part of Isidis Planitia, in December 2003, when contact with the craft was lost. In January 2015, NASA reported the Beagle 2 had been found on the surface in Isidis Planitia (location is about 11.5265 N and 90. | + | The [[Beagle 2]] lander was about to land in the quadrangle, particularly in the eastern part of Isidis Planitia, in December 2003, when contact with the craft was lost. In January 2015, NASA reported the Beagle 2 had been found on the surface in Isidis Planitia (location is about 11.5265 N and 90.4295 E.<ref name="TW-20150116"><nowiki>{{cite web |last=Ellison |first=Doug |title=re Beagle 2 location on Mars => "Using HiView on image ESP_039308_1915_COLOR.JP2 I get 90.4295E 11.5265N" |url=</nowiki>https://twitter.com/doug_ellison/status/556201983443357696 |date=16 January 2015 |work=Twitter & [[JPL]] |</ref> <ref name="NASA-20150116-TG">Grecicius |first1=Tony |last2=Dunbar |first2=Brian |title=Components of Beagle 2 Flight System on Mars |url=http://www.nasa.gov/jpl/mars/pia19106/ |date=16 January 2015 |work=NASA </ref> High-resolution images captured by the [[Mars Reconnaissance Orbiter]] identified the lost probe, which appears to be intact.<ref>Webster |first=Guy |title='Lost' 2003 Mars Lander Found by Mars Reconnaissance Orbiter |url=http://www.nasa.gov/jpl/lost-2003-mars-lander-found-by-mars-reconnaissance-orbiter/ |date=16 January 2015 |work=NASA |</ref> <ref>https://www.nytimes.com/2015/01/17/science/space/missing-lander-beagle-2-finally-located-on-mars.html |date=16 January 2015 |work=[[The New York Times]]</ref> <ref name="BBC-20150116">Amos |first=Jonathan |title=Lost Beagle2 probe found 'intact' on Mars |url=https://www.bbc.co.uk/news/science-environment-30784886 |date=16 January 2015 |work=[[BBC]] </ref> |
| − | == Craters == | + | ==Craters== |
| − | |||
| − | + | [[File: ESP 046046 2095craterandejecta.jpg|thumb|500px|center|Crater and ejecta, as seen by HiRISE under [[HiWish program]]]] | |
| − | + | [[File: 46046 2095crater.jpg|thumb|400px|left|Close view crater and ejecta]] | |
| − | |||
| − | + | [[File: 46046 2095craterclose.jpg|thumb|500px|center|Close view of top of crater wall. Unusual pointed formations visible]] | |
| − | 46046 | ||
| − | |||
| − | |||
| − | + | Some craters in the Amenthes region (as well as other parts of Mars) show ejecta around them that have lobes. It is believed that the lobed shape is caused by an impact into water or ice logged ground. Calculations suggest that ice is stable beneath the Martian surface; hence, it is reasonable to think that some asteroids slammed into ice-rich ground. | |
| + | |||
| + | At the equator a stable layer of ice might lie under as much as 1 kilometer of material, but at higher latitudes the ice may be just a few centimeters below the surface. This was proven when the landing rockets on the Phoenix lander blew away surface dust to reveal an ice surface.<ref>http://www.nasa.gov/mission_pages/phoenix/news/phoenix-20080531.html</ref> <ref>http://www.nasa.gov/centers/ames/news/releases/2008/08_108AR_prt.html</ref> The larger an impact crater, the deeper its penetration, a large crater is more likely to have a lobate ejecta since it went down to the ice layer. When even small craters have lobes, the ice level is close to the surface.<ref>http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=31026</ref> This idea would be very important for future colonists on Mars who would like to live near a source of water. | ||
| + | |||
| + | <gallery class="center" widths="380px" heights="360px"> | ||
| + | |||
| + | Image:Lobate ejecta in Amenthes.JPG|Lobate ejecta in Amenthes. Large crater has lobate ejecta, smaller craters do not show such ejecta since the ice layer was not penetrated by the smaller impacts. Such lobate ejecta are accepted as an impact occurring into ice rich ground. There are more of these where there is more ice in the ground--especially in colder places nearer to the poles. The box show the location of a picture that was taken in high resolution with the Mars Global Surveyor. | ||
</gallery> | </gallery> | ||
| − | |||
| − | |||
| − | <gallery class="center" | + | |
| − | Image:Hebrus Valles.JPG| | + | Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.<ref>Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|accessdate=7 March 2011|date=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7</ref> Sometimes craters will display layers. Since the collision that produces a crater is like a powerful explosion, rocks from deep underground are tossed unto the surface. Hence, craters can show us what lies deep under the surface. One crater in the Amenthes quadrangle is believed to be a source of nakhlite [[meteorites]]. A team of researchers found that these particular meteorites came from four different eruptions of lava because they showed different ages. The ages were measured by comparing isotopes of the element [[Argon]]. Since the ages vary from 93 to 1322 million years, the authors concluded that [[volcano]]es grow much more slowly on Mars than the Earth. The wide range of ages mean that Martian volcanoes erupt off and on for a long, long time. Many of the volcanoes on the Earth grow much quicker, as they form at plate boundaries. In contrast, Martian volcanoes probably form from plumes.<ref>Cohen, B., et al. 2017. Taking the pulse of Mars via dating of a plume-fed volcano. Nature Communications. 8, 640.</ref> |
| + | |||
| + | [[File:ESP 054551 2030craterlayers.jpg|thumb|600px|center|Close view of layers in crater wall]] | ||
| + | |||
| + | ==Hebrus Valles== | ||
| + | |||
| + | Hebrus Vales has tributaries, terraces, and teardrop shaped islands. The teardrop shape of the islands tells us what direction the water used to flow. The terraces may be caused by different layers of rocks or from the water being at different levels in the past. Often, the water level in places changes. For example, if the water flows at a high level for a time, it will create a terrace or beach at that level. And then later, if the level drops, a new terrace will be made.<ref>http://themis.asu.edu/zoom-20020603a</ref> These features are common for the rivers of the Earth. | ||
| + | |||
| + | <gallery class="center" widths="190px" heights="180px"> | ||
| + | Image:Hebrus Valles.JPG|Hebrus Valles, as seen by THEMIS. Direction of flow was determined by shape of streamlined islands. Terraces may have been due to separate flood events. | ||
</gallery> | </gallery> | ||
==Streamlined shapes== | ==Streamlined shapes== | ||
| − | |||
| − | <gallery class="center" | + | [[File:ESP 045860 2085streamlined.jpg|thumb|500px|center|Wide view of streamlined shapes, as seen by HiRISE under [[HiWish program]]]] |
| + | |||
| + | Streamlined shapes are formed from erosion by flowing water. Hence, when we see such shapes we know running water was involved. Mars shows many signs all over its surface that it once had much water. Based on the evidence of all these signs of past water, scientists believe that there is a good chance that life arose and thrived early in its history. Interestingly to consider is the possibility that life first began on Mars and then was later transported to the Earth by low angle impacts of asteroids. Many, many meteoites have been found that have been proven to have originated on Mars. Experiments have shown that organisms could survive the journey. So, many of our genes (DNA) may be of Martian origin. If we find chemical evidence of life on Mars, maybe after just a few months of study we will know whether we our decedents of Martian organisms. | ||
| + | |||
| + | [[File:ESP 045860 2085streamlinedbottom.jpg|thumb|400px|center|Close view of streamlined shapes Arrow indicates the direction of past flowing water.]] | ||
| + | |||
| + | <gallery class="center" widths="380px" heights="360px"> | ||
| − | |||
| − | |||
ESP 045860 2085streamlinedmiddle.jpg|Close view of streamlined shapes | ESP 045860 2085streamlinedmiddle.jpg|Close view of streamlined shapes | ||
ESP 045860 2085streamlinedtop.jpg|Close view of streamlined shapes | ESP 045860 2085streamlinedtop.jpg|Close view of streamlined shapes | ||
| + | File:Streamlined forms ESP 068107 2080.jpg|Streamline features | ||
| + | File:Streamlined forms ESP 070772.jpg|Streamlined features as seen by HiRISE under HiWish program | ||
| + | </gallery> | ||
| + | |||
| + | |||
| + | [[File:ESP 054800 2075streamlined.jpg|thumb|500px|center|Another location with streamlined shapes formed by flowing water]] | ||
| − | File:ESP | + | [[File:Streamlined shapes in channel ESP 054919 2015.jpg|600 pxr|Streamlined shapes from rushing flood waters]] |
| − | + | Streamlined shapes from rushing flood waters | |
==Cones== | ==Cones== | ||
| − | |||
| − | + | [[File: ESP 049975 2045cones.jpg|thumb|600px|center|Cones indicated with arrows, as seen by HiRISE under HiWish program ]] | |
| − | ESP 048023 2040conestroughs.jpg|Wide view of cones and trough | + | Cones can have their origin from volcanic methods or from the movement of mud. When a layer of mud is covered over, it may become pressurized and move up, erupting into what we call “mud volcanoes.” They are common in some areas of Mars. Cones seen in the Amenthes quadrangle are probably mud volcanoes. The pictures in this section show some of the cones found in Amenthes. |
| − | 48023 2040coneclose.jpg|Cone next to a trough | + | |
| − | + | [[File:ESP 048050 2025cones.jpg|thumb|400px|center|Another scene with cones]] | |
| − | Image:ESP 035008 2010cones.jpg|Line of cones | + | |
| − | + | ||
| + | [[File:ESP 048023 2040conestroughs.jpg|thumb|300px|left|Wide view of cones and trough]] | ||
| + | |||
| + | [[File:48023 2040coneclose.jpg|thumb|500px|right|Cone next to a trough]] | ||
| + | |||
| + | <gallery class="center" widths="380px" heights="360px"> | ||
| + | |||
| + | Image:ESP 035008 2010cones.jpg|Line of cones | ||
File:570770 2100cones.jpg|Close view of cones, as seen by HiRISE under HiWish program | File:570770 2100cones.jpg|Close view of cones, as seen by HiRISE under HiWish program | ||
| Line 85: | Line 113: | ||
Mesas form when erosion has removed much of the surrounding ground. They are the remains of material that once covered a wide area. | Mesas form when erosion has removed much of the surrounding ground. They are the remains of material that once covered a wide area. | ||
| − | <gallery class="center" | + | <gallery class="center" widths="380px" heights="360px"> |
ESP 050858 2025mesa.jpg|Layered mesa that appears to have a streamlined shape, as seen by HiRISE under HiWish program A channel has cut through a lower layer. | ESP 050858 2025mesa.jpg|Layered mesa that appears to have a streamlined shape, as seen by HiRISE under HiWish program A channel has cut through a lower layer. | ||
ESP 044832 2035mesa.jpg|Layered mesa | ESP 044832 2035mesa.jpg|Layered mesa | ||
| Line 94: | Line 122: | ||
The Amenthes quadrangle is also home to troughs (long narrow depressions) called fossae in the geographical language used for Mars. These troughs form when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano of which Mars has plenty. | The Amenthes quadrangle is also home to troughs (long narrow depressions) called fossae in the geographical language used for Mars. These troughs form when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano of which Mars has plenty. | ||
| − | <gallery class="center" | + | <gallery class="center" widths="380px" heights="360px"> |
| − | Image:ESP 036801 2015amenthespits.jpg|Large pits | + | Image:ESP 036801 2015amenthespits.jpg|Large pits |
| − | Image:ESP 036023 2025amenthestroughtop.jpg|Trough | + | Image:ESP 036023 2025amenthestroughtop.jpg|Trough |
ESP 051781 2035troughs.jpg|Troughs | ESP 051781 2035troughs.jpg|Troughs | ||
| Line 105: | Line 133: | ||
==Channels== | ==Channels== | ||
| − | + | [[File:Scamander Vallis.JPG|thumb|600px|center|Scamander Vallis. [[Dark slope streaks]] may be seen in the image.]] | |
| − | + | ==See also== | |
| − | |||
| − | |||
| − | == | ||
| − | |||
| − | |||
| − | |||
| − | |||
| − | |||
| − | |||
| − | |||
| − | + | *[[Dark slope streaks]] | |
*[[Geography of Mars]] | *[[Geography of Mars]] | ||
*[[High Resolution Imaging Science Experiment (HiRISE)]] | *[[High Resolution Imaging Science Experiment (HiRISE)]] | ||
*[[HiWish program]] | *[[HiWish program]] | ||
*[[How are features on Mars Named?]] | *[[How are features on Mars Named?]] | ||
| + | *[[Mars Global Surveyor]] | ||
| + | *[[Rivers on Mars]] | ||
| + | |||
==References:== | ==References:== | ||
{{Reflist|2}} | {{Reflist|2}} | ||
Latest revision as of 14:17, 23 December 2023
| MC-14 | Amenthes | 0–30° N | 90–135° E | Quadrangles | Atlas |
The Amenthes quadrangle contains features with names like Isidis, Amenthes Fossae, Libya Montes, and Escalente Crater. Nearly all the names of Martian locations are from old writings like the Bible and Homer. Early astronomers gave names to things they saw on Mars. Things were given names and then other names, over and over. Finally the astronomer Giovanni Schiaparelli, after making drawings when Mars was exceptionally close in 1887, assigned the names still in use today, over a hundred years later.[1] [2] Giovanni Schiaparelli is called the Father of Mars—at one point he knew more about Mars than any other living person. The name Amenthes is the Egyptian word for the place where the souls of the dead go.[3]
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.
Contents
Location
The Amenthes quadrangle covers the area from 0° to 30° north latitude and 225° to 270° west longitude (135-90 E). Amenthes quadrangle contains parts of Utopia Planitia, Isidis Planitia, Terra Cimmeria, and Tyrrhena Terra. There are different ways of telling positions on Mars. One can just give coordinates. One can use one of the maps that have been produced form old drawings dating back to Schiaparelli--this is usually done. Here we are going by a system where the surface of Mars is divided into 30 regions, called quadrangles. Nearly all of the quadrangles use the classical names. So, Amenthes quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS). The Amenthes quadrangle is also referred to as MC-14 (Mars Chart-14).[4]
Significant facts
The Amenthes quadrangle contains several features commonplace on Mars. It has dark slope streaks, troughs (fossae), and river valleys (Vallis {word used in planetary geology}) in this quadrangle. This quadrangle contains the Isidis basin, a location where magnesium carbonate was found by Mars Reconnaissance Orbiter. This mineral indicates that water was present and that it was not acidic. This fact increases the chances of life here in the past. Although some organisms can live in an acid environment, most living things do not thrive in an acid environment. The Beagle 2 lander was about to land in the quadrangle, particularly in the eastern part of Isidis Planitia, in December 2003, when contact with the craft was lost. In January 2015, NASA reported the Beagle 2 had been found on the surface in Isidis Planitia (location is about 11.5265 N and 90.4295 E.[5] [6] High-resolution images captured by the Mars Reconnaissance Orbiter identified the lost probe, which appears to be intact.[7] [8] [9]
Craters
Some craters in the Amenthes region (as well as other parts of Mars) show ejecta around them that have lobes. It is believed that the lobed shape is caused by an impact into water or ice logged ground. Calculations suggest that ice is stable beneath the Martian surface; hence, it is reasonable to think that some asteroids slammed into ice-rich ground.
At the equator a stable layer of ice might lie under as much as 1 kilometer of material, but at higher latitudes the ice may be just a few centimeters below the surface. This was proven when the landing rockets on the Phoenix lander blew away surface dust to reveal an ice surface.[10] [11] The larger an impact crater, the deeper its penetration, a large crater is more likely to have a lobate ejecta since it went down to the ice layer. When even small craters have lobes, the ice level is close to the surface.[12] This idea would be very important for future colonists on Mars who would like to live near a source of water.
Lobate ejecta in Amenthes. Large crater has lobate ejecta, smaller craters do not show such ejecta since the ice layer was not penetrated by the smaller impacts. Such lobate ejecta are accepted as an impact occurring into ice rich ground. There are more of these where there is more ice in the ground--especially in colder places nearer to the poles. The box show the location of a picture that was taken in high resolution with the Mars Global Surveyor.
Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.[13] Sometimes craters will display layers. Since the collision that produces a crater is like a powerful explosion, rocks from deep underground are tossed unto the surface. Hence, craters can show us what lies deep under the surface. One crater in the Amenthes quadrangle is believed to be a source of nakhlite meteorites. A team of researchers found that these particular meteorites came from four different eruptions of lava because they showed different ages. The ages were measured by comparing isotopes of the element Argon. Since the ages vary from 93 to 1322 million years, the authors concluded that volcanoes grow much more slowly on Mars than the Earth. The wide range of ages mean that Martian volcanoes erupt off and on for a long, long time. Many of the volcanoes on the Earth grow much quicker, as they form at plate boundaries. In contrast, Martian volcanoes probably form from plumes.[14]
Hebrus Valles
Hebrus Vales has tributaries, terraces, and teardrop shaped islands. The teardrop shape of the islands tells us what direction the water used to flow. The terraces may be caused by different layers of rocks or from the water being at different levels in the past. Often, the water level in places changes. For example, if the water flows at a high level for a time, it will create a terrace or beach at that level. And then later, if the level drops, a new terrace will be made.[15] These features are common for the rivers of the Earth.
Hebrus Valles, as seen by THEMIS. Direction of flow was determined by shape of streamlined islands. Terraces may have been due to separate flood events.
Streamlined shapes
Streamlined shapes are formed from erosion by flowing water. Hence, when we see such shapes we know running water was involved. Mars shows many signs all over its surface that it once had much water. Based on the evidence of all these signs of past water, scientists believe that there is a good chance that life arose and thrived early in its history. Interestingly to consider is the possibility that life first began on Mars and then was later transported to the Earth by low angle impacts of asteroids. Many, many meteoites have been found that have been proven to have originated on Mars. Experiments have shown that organisms could survive the journey. So, many of our genes (DNA) may be of Martian origin. If we find chemical evidence of life on Mars, maybe after just a few months of study we will know whether we our decedents of Martian organisms.
Close view of streamlined shapes
Close view of streamlined shapes
Streamline features
Streamlined features as seen by HiRISE under HiWish program
Streamlined shapes from rushing flood waters
Cones
Cones can have their origin from volcanic methods or from the movement of mud. When a layer of mud is covered over, it may become pressurized and move up, erupting into what we call “mud volcanoes.” They are common in some areas of Mars. Cones seen in the Amenthes quadrangle are probably mud volcanoes. The pictures in this section show some of the cones found in Amenthes.
Line of cones
Close view of cones, as seen by HiRISE under HiWish program
Mesas
Mesas form when erosion has removed much of the surrounding ground. They are the remains of material that once covered a wide area.
Layered mesa that appears to have a streamlined shape, as seen by HiRISE under HiWish program A channel has cut through a lower layer.
Layered mesa
Fossae
The Amenthes quadrangle is also home to troughs (long narrow depressions) called fossae in the geographical language used for Mars. These troughs form when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano of which Mars has plenty.
Large pits
Trough
Troughs
Troughs cutting through mesa, as seen by HiRISE under HiWish program
Channels
See also
- Dark slope streaks
- Geography of Mars
- High Resolution Imaging Science Experiment (HiRISE)
- HiWish program
- How are features on Mars Named?
- Mars Global Surveyor
- Rivers on Mars
References:
- ↑ Macdonald, T. 1971. The origins of Martian Nomenclature. Icarus: 15, 233-240.
- ↑ Glasstone, S. 1968. The Book of Mars. NASA. Washington, D.C
- ↑ Blunck, J. 1982. Mars and its Satellites. Exposition Press. Smithtown, N.Y.
- ↑ 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.
- ↑ {{cite web |last=Ellison |first=Doug |title=re Beagle 2 location on Mars => "Using HiView on image ESP_039308_1915_COLOR.JP2 I get 90.4295E 11.5265N" |url=https://twitter.com/doug_ellison/status/556201983443357696 |date=16 January 2015 |work=Twitter & JPL |
- ↑ Grecicius |first1=Tony |last2=Dunbar |first2=Brian |title=Components of Beagle 2 Flight System on Mars |url=http://www.nasa.gov/jpl/mars/pia19106/ |date=16 January 2015 |work=NASA
- ↑ Webster |first=Guy |title='Lost' 2003 Mars Lander Found by Mars Reconnaissance Orbiter |url=http://www.nasa.gov/jpl/lost-2003-mars-lander-found-by-mars-reconnaissance-orbiter/ |date=16 January 2015 |work=NASA |
- ↑ https://www.nytimes.com/2015/01/17/science/space/missing-lander-beagle-2-finally-located-on-mars.html |date=16 January 2015 |work=The New York Times
- ↑ Amos |first=Jonathan |title=Lost Beagle2 probe found 'intact' on Mars |url=https://www.bbc.co.uk/news/science-environment-30784886 |date=16 January 2015 |work=BBC
- ↑ http://www.nasa.gov/mission_pages/phoenix/news/phoenix-20080531.html
- ↑ http://www.nasa.gov/centers/ames/news/releases/2008/08_108AR_prt.html
- ↑ http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=31026
- ↑ Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ%7Caccessdate=7 March 2011|date=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7
- ↑ Cohen, B., et al. 2017. Taking the pulse of Mars via dating of a plume-fed volcano. Nature Communications. 8, 640.
- ↑ http://themis.asu.edu/zoom-20020603a
