Difference between revisions of "Cebrenia quadrangle"

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The Cebrenia quadrangle is one of a series of 30 quadrangle maps of Mars. The quadrangle  covers  from 120° to 180° east longitude (180° to 240° west longitude) and from 30° to 65° north latitude. It is also referred to as MC-7 (Mars Chart-7).<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>  Parts of Utopia Planitia and Arcadia Planitia lie in the Cebrenia quadrangle. <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 Cebrenia quadrangle is one of a series of 30 quadrangle maps of Mars. The quadrangle  covers  from 120° to 180° east longitude (180° to 240° west longitude) and from 30° to 65° north latitude. It is also referred to as MC-7 (Mars Chart-7).<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>  Parts of Utopia Planitia and Arcadia Planitia lie in the Cebrenia quadrangle. <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>
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This article aims to describe the location and major features of this quadrangle.  When you finish reading it, you will know what it looks like from orbit and from the surface.  Some HiRISE images may even show how it looks from the altitude of an airplane or a helicopter.
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This article aims to describe the major features of this quadrangle.  When you finish reading it, you will know what it looks like from orbit and from the surface.  Some HiRISE images may even show how it looks from the altitude of an airplane or a helicopter.
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==Origin of name==
 
==Origin of name==
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Cebrenia is a classical albedo feature on Mars. The feature is named after Cebrenia, a country near ancient Troy. The name was approved by the International Astronomical Union (IAU) in 1958.<ref>http://planetarynames.wr.usgs.gov/Feature/1095</ref> <ref>https://planetarynames.wr.usgs.gov/</ref>
 
Cebrenia is a classical albedo feature on Mars. The feature is named after Cebrenia, a country near ancient Troy. The name was approved by the International Astronomical Union (IAU) in 1958.<ref>http://planetarynames.wr.usgs.gov/Feature/1095</ref> <ref>https://planetarynames.wr.usgs.gov/</ref>
  
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The major landscape features of the Cebrenia quadrangle are the large craters Mie and Stokes, a volcano called Hecates Tholus, and a group of mountains, named  the Phlegra Montes.  Most of the quadrangle is characterized as flat and smooth; hence, the rather large craters Mie and Stokes really stand out.  The Galaxias Region is classified as an area of chaos; the ground just seems to have collapsed there.
 
The major landscape features of the Cebrenia quadrangle are the large craters Mie and Stokes, a volcano called Hecates Tholus, and a group of mountains, named  the Phlegra Montes.  Most of the quadrangle is characterized as flat and smooth; hence, the rather large craters Mie and Stokes really stand out.  The Galaxias Region is classified as an area of chaos; the ground just seems to have collapsed there.
 
Some features found here are very common on Mars, but rare—if they exist at all—on the Earth.  Pedestal craters, lineated valley fill (LVF), latitude dependent mantle (LDM), various-shaped layered features, and brain terrain are in this category.  As on Earth, this region of Mars displays channels, layered terrain, cones, impact craters, gullies, and evidence of glaciers.<ref>https://en.wikipedia.org/wiki/Cebrenia_quadrangle#Physiography_and_geology</ref>
 
Some features found here are very common on Mars, but rare—if they exist at all—on the Earth.  Pedestal craters, lineated valley fill (LVF), latitude dependent mantle (LDM), various-shaped layered features, and brain terrain are in this category.  As on Earth, this region of Mars displays channels, layered terrain, cones, impact craters, gullies, and evidence of glaciers.<ref>https://en.wikipedia.org/wiki/Cebrenia_quadrangle#Physiography_and_geology</ref>
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Viking 2  landed near MieCrater on September 3, 1976. Its landing coordinates were 48° N and 226° W (134 E).<ref>''Ezell E. K., Ezell L. N.'' [http://www.hq.nasa.gov/office/pao/History/SP-4212/ch10.html On Mars: Exploration of the Red Planet. 1958-1978. (Chapter 10)]. The NASA History Series. Scientific and Technical Information Branch, 1984. NASA, Washington, D.C.</ref>
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Viking 2  landed near Mie Crater on September 3, 1976. Its landing coordinates were 48° N and 226° W (134 E).<ref>''Ezell E. K., Ezell L. N.'' [http://www.hq.nasa.gov/office/pao/History/SP-4212/ch10.html On Mars: Exploration of the Red Planet. 1958-1978. (Chapter 10)]. The NASA History Series. Scientific and Technical Information Branch, 1984. NASA, Washington, D.C.</ref>
  
 
==[[Hecates Tholus]]==
 
==[[Hecates Tholus]]==
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[[Image:MOLA hecates tholus.jpg |thumb|300px|center| Tographic map of area around Hecates Tholus]]
 
[[Image:MOLA hecates tholus.jpg |thumb|300px|center| Tographic map of area around Hecates Tholus]]
 
  [[Image:27108hecatechannels.jpg |thumb|right|300px|Lava channels on Hecates Tholus]]
 
  [[Image:27108hecatechannels.jpg |thumb|right|300px|Lava channels on Hecates Tholus]]
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==Craters==
 
==Craters==
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Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.<ref name="Kieffer1992">{{cite book|author=Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|accessdate=7 March 2011|year=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 onto the surface.  Consequently, craters can tell us what lies deep under the surface.
 
  
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Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.<ref>Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|accessdate=7 March 2011|year=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 onto the surface.  Consequently, craters can tell us what lies deep under the surface.
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File:ESP 056607 2170layers.jpg|Crater showing layers, as seen by HiRISE under HiWish program
 
File:ESP 056607 2170layers.jpg|Crater showing layers, as seen by HiRISE under HiWish program
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==Gullies==
 
==Gullies==
  
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Gullies occur on steep slopes, especially on the walls of craters. Gullies are believed to be relatively young because they have few, if any craters. Moreover, they lie on top of sand dunes which themselves are considered to be quite young. Usually, each gully has an alcove, channel, and apron.<ref>Edgett |first1= K.  |last2= Malin |first2= M. C. |last3= Williams |first3= R. M. E. |last4= Davis |first4= S. D. |date= 2003 |title=  Polar-and middle-latitude martian gullies: A view from MGS MOC after 2 Mars years in the mapping orbit |journal=  Lunar Planet. Sci. |volume=34  |at=p. 1038, Abstract 1038 | url=http://www.lpi.usra.edu/meetings/lpsc2003/pdf/1038.pdf |</ref> <ref>Dickson | first1 = J | last2 = Head | first2 = J | last3 = Kreslavsky | first3 = M | title = Martian gullies in the southern mid-latitudes of Mars: Evidence for climate-controlled formation of young fluvial features based upon local and global topography | doi = 10.1016/j.icarus.2006.11.020 | </ref> <ref>http://www.planetary.brown.edu/pdfs/3138.pdf | date = 2007 | pages = 315–323 | volume = 188 | issue = 2 | journal = Icarus | </ref>
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For years, many believed that gullies were formed by running water, but further observations demonstrate that they may be formed by dry ice.<ref>http://www.jpl.nasa.gov/news/news.php?release=2014-226</ref> <ref>http://hirise.lpl.arizona.edu/ESP_032078_1420</ref> <ref>http://www.space.com/26534-mars-gullies-dry-ice.html</ref>  In some years frost, perhaps as thick as 1 meter, triggers avalanches. This frost contains mostly dry ice, but also has tiny amounts of water ice.<ref>http://spaceref.com/mars/frosty-gullies-on-mars.html</ref>
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File:Chincoteague Crater.jpg|Chincoteague Crater
 
File:Chincoteague Crater.jpg|Chincoteague Crater
 
File:Chincoteague Crater close up.jpg|Close-up of Chincoteague Crater, as seen by HiRISE  Gullies are visible.  Gullies may be created by water and/or dry ice moving down the crater walls.  The exact cause is debatable at present.
 
File:Chincoteague Crater close up.jpg|Close-up of Chincoteague Crater, as seen by HiRISE  Gullies are visible.  Gullies may be created by water and/or dry ice moving down the crater walls.  The exact cause is debatable at present.
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A  pedestal crater is an impact crater which has  its ejecta sitting above the surrounding terrain.  This forms a raised platform (like a pedestal). These craters are produced when an impact crater ejects material that forms an erosion-resistant layer at the top, thus causing the immediate area to erode more slowly than the rest of the region. Some pedestals have been accurately measured to be hundreds of meters above the surrounding area. This means that hundreds of meters of material were eroded away. The result is that both the crater and its ejecta blanket stand above the surroundings. Pedestal craters were first observed during the Mariner missions.<ref>http://hirise.lpl.eduPSP_008508_1870</ref> <ref>Bleacher, J. and S. Sakimoto. ''Pedestal Craters, A Tool For Interpreting Geological Histories and Estimating Erosion Rates''.  LPSC</ref>  <ref>http://themis.asu.edu/feature_utopiacraters</ref> <ref>McCauley, John F. (December 1972). "Mariner 9 Evidence for Wind Erosion in the Equatorial and Mid-Latitude Regions of Mars". Journal of Geophysical Research. 78 (20): 4123–4137(JGRHomepage). </ref>  Much of the material under the pedestal crater’ ejecta may be ice.  These types of craters may be useful for finding sources of water ice since they can be easily spotted and mapped from orbit.
 
A  pedestal crater is an impact crater which has  its ejecta sitting above the surrounding terrain.  This forms a raised platform (like a pedestal). These craters are produced when an impact crater ejects material that forms an erosion-resistant layer at the top, thus causing the immediate area to erode more slowly than the rest of the region. Some pedestals have been accurately measured to be hundreds of meters above the surrounding area. This means that hundreds of meters of material were eroded away. The result is that both the crater and its ejecta blanket stand above the surroundings. Pedestal craters were first observed during the Mariner missions.<ref>http://hirise.lpl.eduPSP_008508_1870</ref> <ref>Bleacher, J. and S. Sakimoto. ''Pedestal Craters, A Tool For Interpreting Geological Histories and Estimating Erosion Rates''.  LPSC</ref>  <ref>http://themis.asu.edu/feature_utopiacraters</ref> <ref>McCauley, John F. (December 1972). "Mariner 9 Evidence for Wind Erosion in the Equatorial and Mid-Latitude Regions of Mars". Journal of Geophysical Research. 78 (20): 4123–4137(JGRHomepage). </ref>  Much of the material under the pedestal crater’ ejecta may be ice.  These types of craters may be useful for finding sources of water ice since they can be easily spotted and mapped from orbit.
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File:ESP 047772 2210pedestal.jpg|Pedestal crater  
 
File:ESP 047772 2210pedestal.jpg|Pedestal crater  
 
File:ESP 048021 2130pedestal.jpg|Pedestal crater
 
File:ESP 048021 2130pedestal.jpg|Pedestal crater
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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>  In fact, a study published in June 2017, estimated 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>  In fact, a study published in June 2017, estimated 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>
  
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File:47653 2150ctxchannel.jpg| Hrad Vallis, as seen by CTX  Photo labeled with layers, streamlined forms, and arrow indicating direction water flowed.
 
File:47653 2150ctxchannel.jpg| Hrad Vallis, as seen by CTX  Photo labeled with layers, streamlined forms, and arrow indicating direction water flowed.
 
File:ESP 052738 2135channel.jpg|Channel, as seen by HiRISE under HiWish program
 
File:ESP 052738 2135channel.jpg|Channel, as seen by HiRISE under HiWish program
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Large amounts of water ice are believed to be present just under the surface of Mars.  Some channels lie near volcanic areas.  When hot subsurface magma comes close to this ice, large amounts of liquid water and mud may be formed. Hrad Vallis in the Cebrenia quadrangle is close to the large volcano, Elysium Mons.  It may have supplied heat to melt ice and  make the channel.  Hrad Vallis is pictured below.<ref>http://themis.asu.edu/zoom-20020715a.html</ref>
 
Large amounts of water ice are believed to be present just under the surface of Mars.  Some channels lie near volcanic areas.  When hot subsurface magma comes close to this ice, large amounts of liquid water and mud may be formed. Hrad Vallis in the Cebrenia quadrangle is close to the large volcano, Elysium Mons.  It may have supplied heat to melt ice and  make the channel.  Hrad Vallis is pictured below.<ref>http://themis.asu.edu/zoom-20020715a.html</ref>
  
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File:Hrad Vallis in Cebrenia2.jpg|Hrad Vallis may have been formed when the large Elysium Mons volcanic complex melted ground ice, as seen by THEMIS.
 
File:Hrad Vallis in Cebrenia2.jpg|Hrad Vallis may have been formed when the large Elysium Mons volcanic complex melted ground ice, as seen by THEMIS.
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==Layered structures==
 
==Layered structures==
  
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Some locations on Mars display layered features in craters, depressions, and next to mesas.  These are probably the remains of materials that once covered a wide region.  They may mostly consist of latitude dependent mantle which falls from the sky as ice-rich particles.
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Some locations on Mars display layered features in craters, depressions, and leaning on mesas.  These are probably the remains of materials that once covered a wide region.  They may mostly consist of latitude dependent mantle which falls from the sky as ice-rich particles.
  
  
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Another ice-rich feature is called lineated valley fill (LVF). <ref>Carr, M. 2006. The Surface of Mars.  Cambridge University Press. ISBN|978-0-521-87201-0</ref> <ref>Squyres, S.  1978.  Martian fretted terrain:  Flow of erosional debris.  Icarus: 34. 600-613.</ref> <ref>Levy. et al. 2007.  Lineated valley fill and lobate debris apron stratigraphy in Nilosyrtis Mensae, Mars: Evidence for phases of glacial modification of the dichotomy boundary. J. Geophys. Res. 112</ref>  It covers many of the wide, flat valley floors of fretted terrain.  Probably formed from the interaction of glaciers coming out of valleys and of mesas eroding, it has similar surface appearance of other supposed glaciers, including LDA.  It looks like the human brain.  Since the material covering ice is shaped into something resembling the human brain, it is named brain terrain.  Brain terrain starts to form with cracks in the ice-rich surface.  [[Sublimation]] along the cracks turns the cracks into small valleys. <ref>Mellon, M.  1997.  Small-scale polygonal features on Mars:  Seasonal thermal contraction cracks in permafrost.  J. Geophysical Res: 102. 25,617-625,628.</ref> <ref>Levy, J. et al.  2009.  Concentric crater fill in Utopia Planitia:  History and interaction between glacial "brain terrain" and periglacial processes.  Icarus: 202.  462-476.</ref>  <ref name="Souness, C 2013">cite journal | author = Souness C., Hubbard B. | year = 2013 | title = An alternative interpretation of late Amazonian ice flow: Protonilus Mensae, Mars | url = | journal = Icarus | volume = 225 | issue = | pages = 495–505 | doi=10.1016/j.icarus.2013.03.030 |</ref> <ref name="Noach">cite journal |author1=Head, J.  |author2=D. Marchant  |lastauthoramp=yes| date = 2006 | title = Modification of the walls of a Noachian crater in northern Arabia Terra (24E, 39N) during mid-latitude Amazonian glacial epochs on Mars:  Nature and evolution of lobate debris aprons and their relationships to lineated valley fill and glacial systems | journal = Lunar Planet. Sci | volume =  37 | page =  Abstract # 1126</ref> <ref>cite journal | author = Kress, A., J. Head | date =  2008 | title =  Ring-mold craters in lineated valley fill and lobate debris aprons on Mars:  Evidence for subsurface glacial ice | journal = Geophys. Res. Lett. | volume = 35 | page = L23206–8 | doi=10.1029/2008gl035501|</ref> <ref>cite journal | author = Baker, D. | date = 2010 | title = Flow patterns of lobate debris aprons and lineated valley fill north of Ismeniae Fossae, Mars:  Evidence for extensive mid-latitude glaciation in the Late Amazonian | journal = Icarus | volume = 207 | pages = 186–209 | doi = 10.1016/j.icarus.2009.11.017 | last2 = Head | first2 = James W. | last3 = Marchant | first3 = David R. </ref>  <ref>cite journal |author1=Kress., A.  |author2=J. Head  |lastauthoramp=yes| date = 2009 | title = Ring-mould craters on lineated valley fill, lobate debris aprons, and concentric crater fill on Mars:  Implications for near-surface structure, composition, and age | journal = Lunar Planet. Sci | volume = 40 | page = abstract 1379</ref>
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Another ice-rich feature is called lineated valley fill (LVF). <ref>Carr, M. 2006. The Surface of Mars.  Cambridge University Press. ISBN|978-0-521-87201-0</ref> <ref>Squyres, S.  1978.  Martian fretted terrain:  Flow of erosional debris.  Icarus: 34. 600-613.</ref> <ref>Levy. et al. 2007.  Lineated valley fill and lobate debris apron stratigraphy in Nilosyrtis Mensae, Mars: Evidence for phases of glacial modification of the dichotomy boundary. J. Geophys. Res. 112</ref>  It covers many of the wide, flat valley floors of fretted terrain.  LVF may have formed from the interaction of glaciers coming out of valleys and from mesas eroding, it has similar surface appearance of other supposed glaciers, including LDA.  The surface resembles the human brain.  Since the material covering ice is shaped into something resembling the human brain, it is named brain terrain.  Brain terrain starts to form with cracks in the ice-rich surface.  [[Sublimation]] along the cracks turns the cracks into small valleys. <ref>Mellon, M.  1997.  Small-scale polygonal features on Mars:  Seasonal thermal contraction cracks in permafrost.  J. Geophysical Res: 102. 25,617-625,628.</ref> <ref>Levy, J. et al.  2009.  Concentric crater fill in Utopia Planitia:  History and interaction between glacial "brain terrain" and periglacial processes.  Icarus: 202.  462-476.</ref>  <ref name="Souness, C 2013">cite journal | author = Souness C., Hubbard B. | year = 2013 | title = An alternative interpretation of late Amazonian ice flow: Protonilus Mensae, Mars | url = | journal = Icarus | volume = 225 | issue = | pages = 495–505 | doi=10.1016/j.icarus.2013.03.030 |</ref> <ref name="Noach">cite journal |author1=Head, J.  |author2=D. Marchant  |lastauthoramp=yes| date = 2006 | title = Modification of the walls of a Noachian crater in northern Arabia Terra (24E, 39N) during mid-latitude Amazonian glacial epochs on Mars:  Nature and evolution of lobate debris aprons and their relationships to lineated valley fill and glacial systems | journal = Lunar Planet. Sci | volume =  37 | page =  Abstract # 1126</ref> <ref>cite journal | author = Kress, A., J. Head | date =  2008 | title =  Ring-mold craters in lineated valley fill and lobate debris aprons on Mars:  Evidence for subsurface glacial ice | journal = Geophys. Res. Lett. | volume = 35 | page = L23206–8 | doi=10.1029/2008gl035501|</ref> <ref>cite journal | author = Baker, D. | date = 2010 | title = Flow patterns of lobate debris aprons and lineated valley fill north of Ismeniae Fossae, Mars:  Evidence for extensive mid-latitude glaciation in the Late Amazonian | journal = Icarus | volume = 207 | pages = 186–209 | doi = 10.1016/j.icarus.2009.11.017 | last2 = Head | first2 = James W. | last3 = Marchant | first3 = David R. </ref>  <ref>cite journal |author1=Kress., A.  |author2=J. Head  |lastauthoramp=yes| date = 2009 | title = Ring-mould craters on lineated valley fill, lobate debris aprons, and concentric crater fill on Mars:  Implications for near-surface structure, composition, and age | journal = Lunar Planet. Sci | volume = 40 | page = abstract 1379</ref>
  
 
[[File:57212 2110brainsface.jpg|thumb|300px|left|Brain terrain on crater floor, as seen by HiRISE under HiWish program  Brain terrain forms when cracks form and get larger.]]
 
[[File:57212 2110brainsface.jpg|thumb|300px|left|Brain terrain on crater floor, as seen by HiRISE under HiWish program  Brain terrain forms when cracks form and get larger.]]
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Some areas of Mars are classified as regions of “Chaos.”  The ground seems to have collapsed.  Often large blocks and hills are present in abundance.  Many have large outflow channels associated with them.  Galaxias Chaos in the Cebrenia quadrangle is different from most other chaotic regions.  It does not have outflow channels, and it does not show a great elevation difference between it and the neighboring land area.  Research by Pedersen and Head, published in 2010, suggests that Galaxias Chaos is the site of a volcanic flow that buried an ice-rich layer.  That buried layer is a residue from water-rich materials deposited by large floods.<ref>Kreslavsky, Mikhail A. (2002). "Fate of outflow channel effluents in the northern lowlands of Mars: The Vastitas Borealis Formation as a sublimation residue from frozen ponded bodies of water". Journal of Geophysical Research.</ref> <ref>Carr, Michael H. (2003). "Oceans on Mars: An assessment of the observational evidence and possible fate" (PDF). Journal of Geophysical Research. 108 (E5): 5042.</ref>
 
Some areas of Mars are classified as regions of “Chaos.”  The ground seems to have collapsed.  Often large blocks and hills are present in abundance.  Many have large outflow channels associated with them.  Galaxias Chaos in the Cebrenia quadrangle is different from most other chaotic regions.  It does not have outflow channels, and it does not show a great elevation difference between it and the neighboring land area.  Research by Pedersen and Head, published in 2010, suggests that Galaxias Chaos is the site of a volcanic flow that buried an ice-rich layer.  That buried layer is a residue from water-rich materials deposited by large floods.<ref>Kreslavsky, Mikhail A. (2002). "Fate of outflow channel effluents in the northern lowlands of Mars: The Vastitas Borealis Formation as a sublimation residue from frozen ponded bodies of water". Journal of Geophysical Research.</ref> <ref>Carr, Michael H. (2003). "Oceans on Mars: An assessment of the observational evidence and possible fate" (PDF). Journal of Geophysical Research. 108 (E5): 5042.</ref>
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Since the upper lava cap would not be supported evenly all over, it would crack.  Along the cracks [[sublimation]] of water into the thin Martian atmosphere would be more intense.  A blocky terrain that is typical of chaos would eventually develop.  The sublimation process may have been facilitated by heat  from magma movements.  There are volcanoes, namely Elysium Montes and Hecates Tholus, close by which probably are surrounded by dikes, which would have heated the ground.  Dikes occur when magma goes into cracks and weak areas rather than to the top of a volcano.  They are widespread around most volcanoes.  Ship rock, New Mexico contains typical dikes that have been exposed by erosion.  Also, a warmer period in the past would have increased the amount of water sublimating from the ground.<ref>Pedersen, G. and J. Head. 2011. Chaos formation by sublimation of volatile-rich substrate: evidence from Galaxias Chaos, Mars. Icarus. 211: 316-329.</ref>
+
Since the upper lava cap would not be supported evenly all over, it would crack.  Along the cracks [[sublimation]] of water into the thin Martian atmosphere would be more intense.  A blocky terrain that is typical of chaos would eventually develop.  The sublimation process may have been facilitated by heat  from magma movements.  There are volcanoes, namely Elysium Montes and Hecates Tholus, close by which probably are surrounded by dikes, which would have heated the ground.  Dikes occur when magma goes into cracks and weak areas rather than to the top of a volcano.  They are widespread around most volcanoes.  Shiprock, New Mexico contains typical dikes that have been exposed by erosion.  Also, a warmer period in the past would have increased the amount of water sublimating from the ground.<ref>Pedersen, G. and J. Head. 2011. Chaos formation by sublimation of volatile-rich substrate: evidence from Galaxias Chaos, Mars. Icarus. 211: 316-329.</ref>
  
 
==Ice exposed in new craters==
 
==Ice exposed in new craters==
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==Cones==
 
==Cones==
  
−
<gallery class="center" widths="190px" heights="180px">
+
<gallery class="center" widths="380px" heights="360px">
 
File:ESP 047376 2185cones.jpg|Cones  Some cones are thought to be mud volcanoes.  Since the mud has been brought up from some depth it may contain remains of life that were protected from radiation at the surface.
 
File:ESP 047376 2185cones.jpg|Cones  Some cones are thought to be mud volcanoes.  Since the mud has been brought up from some depth it may contain remains of life that were protected from radiation at the surface.
 
</gallery>
 
</gallery>
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                                                           View of surface around Viking 2
 
                                                           View of surface around Viking 2
  
−
Minerals detected in the soil were similar to those produced from the weathering of basaltic lavas on Earth.  Dirt at this site contained abundant silicon and iron, in addition to significant amounts of magnesium, aluminum, sulfur, calcium, and titanium.  Strontium and yttrium were found in trace amounts.  Potassium was 5 times lower than the average in the Earth's crust. Sulfur and chlorine were similar to compounds that remain after sea water evaporates.  Sulfur was more concentrated in the top crust of the soil than in the underlying bulk soil.  Sulfur could be in the form of sulfates of sodium, magnesium, calcium, or iron.  Iron sulfide is also possible. <ref>Clark, B. et al.  1976.  Inorganic Analysis of Martian Samples at the Viking Landing Sites.  Science:  194. 1283-1288.</ref> Elements in the soil were found with an X-ray fluorescence spectrometer.<ref>https://nssdc.gsfc.nasa.gov/nmc/spacecraft/display.action?id=1975-083C</ref>  Mineral models suggest that the soil could be a mixture of about 90% iron-rich clay, about 10% magnesium sulfate  (kieserite?), about 5% carbonate (calcite), and about 5% iron oxides (hematite, magnetite, goethite?).  These minerals are typical weathering products of mafic igneous rocks.  The dark, igneous rock basalt is believed to make up much of the surface of Mars, as it does for the Earth.<ref>Baird, A.  et al.  1976.  Mineralogic and Petrologic Implications of Viking Geochemical Results From Mars: Interim Report.  Science: 194. 1288-1293.</ref> <ref>Toulmin III, P. et al.  1977.  Geochemical and Mineralogical Interpretation of the Viking Inorganic Chemical Results.  Journal of Geophysical Research: 82. 4625-4634.</ref> <ref>Clark, B. et al.  1982.  Chemical Composition of Martian Fines.  Journal of Geophysical Research: 87. 10059-10097</ref>
+
Minerals detected in the soil were similar to those produced from the weathering of basaltic lavas on Earth.  Dirt at this site contained abundant silicon and iron, in addition to significant amounts of magnesium, aluminum, sulfur, calcium, and titanium.  Strontium and yttrium were found in trace amounts.  Potassium was 5 times lower than the average in the Earth's crust. Sulfur and chlorine were similar to compounds that remain after sea water evaporates.  Sulfur was more concentrated in the top crust of the soil than in the underlying bulk soil.  Sulfur could be in the form of sulfates of sodium, magnesium, calcium, or iron.  Iron sulfide is also possible. <ref>Clark, B. et al.  1976.  Inorganic Analysis of Martian Samples at the Viking Landing Sites.  Science:  194. 1283-1288.</ref>
 +
 
 +
Elements in the soil were found with an X-ray fluorescence spectrometer.<ref>https://nssdc.gsfc.nasa.gov/nmc/spacecraft/display.action?id=1975-083C</ref>  Mineral models suggest that the soil could be a mixture of about 90% iron-rich clay, about 10% magnesium sulfate  (kieserite?), about 5% carbonate (calcite), and about 5% iron oxides (hematite, magnetite, goethite?).  These minerals are typical weathering products of mafic igneous rocks.   
 +
 
 +
The dark, igneous rock basalt is believed to make up much of the surface of Mars, as it does for the Earth.<ref>Baird, A.  et al.  1976.  Mineralogic and Petrologic Implications of Viking Geochemical Results From Mars: Interim Report.  Science: 194. 1288-1293.</ref> <ref>Toulmin III, P. et al.  1977.  Geochemical and Mineralogical Interpretation of the Viking Inorganic Chemical Results.  Journal of Geophysical Research: 82. 4625-4634.</ref> <ref>Clark, B. et al.  1982.  Chemical Composition of Martian Fines.  Journal of Geophysical Research: 87. 10059-10097</ref>
 +
 
 
Studies with magnets aboard the Viking  landers indicated that the soil is between 3 and 7 percent magnetic materials by weight.  The magnetic chemicals could be magnetite and maghemite.  These could come from the weathering of basalt rock.<ref>Hargraves, R. et al. 1976.  Viking Magnetic Properties Investigation: Further Results.  Science: 194.  1303-1309.</ref> <ref>Arvidson, R, A. Binder, and K. Jones.  The Surface of Mars.  Scientific American</ref>  
 
Studies with magnets aboard the Viking  landers indicated that the soil is between 3 and 7 percent magnetic materials by weight.  The magnetic chemicals could be magnetite and maghemite.  These could come from the weathering of basalt rock.<ref>Hargraves, R. et al. 1976.  Viking Magnetic Properties Investigation: Further Results.  Science: 194.  1303-1309.</ref> <ref>Arvidson, R, A. Binder, and K. Jones.  The Surface of Mars.  Scientific American</ref>  
  
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*https://www.youtube.com/watch?v=w1s5buM6iyk Cebrenia quadrangle - Video Learning - WizScience.com
 
*https://www.youtube.com/watch?v=w1s5buM6iyk Cebrenia quadrangle - Video Learning - WizScience.com
 
*https://www.youtube.com/watch?v=CoMbVt7qdH8 Mars Clips 15 The Cebrenia Region Viking 2 Lander video  
 
*https://www.youtube.com/watch?v=CoMbVt7qdH8 Mars Clips 15 The Cebrenia Region Viking 2 Lander video  
 +
 +
 +
* [https://www.sciencedirect.com/science/article/pii/S0019103520305121#f0010  Gallagher. c.  et al.  In press 2020.  Landforms indicative of regional warm based glaciation, Phlegra Montes, Mars.  Icarus ]
  
 
[[Category:Mars Atlas]]
 
[[Category:Mars Atlas]]

Latest revision as of 15:15, 3 November 2020

Mars topography (MOLA dataset) HiRes (1).jpg
MC-07 Cebrenia quadrangle 30–65° N 120°–180° E Quadrangles Atlas
  • USGS-Mars-MC-7-CebreniaRegion-mola.png

  • Image of the Cebrenia Quadrangle (MC-7). The northwest contains relatively smooth plains; the southeast contains Hecates Tholus (one of three Elysium shield volcanoes) and Phlegra Montes (a ridge system).

The Cebrenia quadrangle is one of a series of 30 quadrangle maps of Mars. The quadrangle covers from 120° to 180° east longitude (180° to 240° west longitude) and from 30° to 65° north latitude. It is also referred to as MC-7 (Mars Chart-7).[1] Parts of Utopia Planitia and Arcadia Planitia lie in the Cebrenia quadrangle. [2]

This article aims to describe the major features of this quadrangle. When you finish reading it, you will know what it looks like from orbit and from the surface. Some HiRISE images may even show how it looks from the altitude of an airplane or a helicopter.

Origin of name

Cebrenia is a classical albedo feature on Mars. The feature is named after Cebrenia, a country near ancient Troy. The name was approved by the International Astronomical Union (IAU) in 1958.[3] [4]

Major Features

The major landscape features of the Cebrenia quadrangle are the large craters Mie and Stokes, a volcano called Hecates Tholus, and a group of mountains, named the Phlegra Montes. Most of the quadrangle is characterized as flat and smooth; hence, the rather large craters Mie and Stokes really stand out. The Galaxias Region is classified as an area of chaos; the ground just seems to have collapsed there. Some features found here are very common on Mars, but rare—if they exist at all—on the Earth. Pedestal craters, lineated valley fill (LVF), latitude dependent mantle (LDM), various-shaped layered features, and brain terrain are in this category. As on Earth, this region of Mars displays channels, layered terrain, cones, impact craters, gullies, and evidence of glaciers.[5] Viking 2 landed near Mie Crater on September 3, 1976. Its landing coordinates were 48° N and 226° W (134 E).[6]

Hecates Tholus

Scientists believe that Hecates Tholus erupted explosively about 350 million years ago, which is a not that long ago for Mars. These eruptions made depressions on the sides of the volcano. And just five million years ago, glacial deposits formed inside these depressions. Some valleys on Hecates show a parallel drainage pattern.[7] Hecates Tholus is in the Elysium Volcanic Region; the two other volcanoes there are Elysium Mons and Albor Tholus.

Hecates Tholus, as seen by Mars Global Surveyor.
Tographic map of area around Hecates Tholus
Lava channels on Hecates Tholus

Craters

Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.[8] Sometimes craters will display layers. Since the collision that produces a crater is like a powerful explosion, rocks from deep underground are tossed onto the surface. Consequently, craters can tell us what lies deep under the surface.

  • Crater showing layers, as seen by HiRISE under HiWish program

  • Mie Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Viking II landed near Mie Crater in 1976.

  • Craters with layered mounds and tall, sharp rims These mounds may be similar to the mountain, Mt. Sharp, in Gale Crater where the Curiosity Rover is exploring.

Group of secondary craters These are produced when a big impact throws boulders high in the air. They often land in groups and can be identified by their identical ages.

Gullies

Gullies occur on steep slopes, especially on the walls of craters. Gullies are believed to be relatively young because they have few, if any craters. Moreover, they lie on top of sand dunes which themselves are considered to be quite young. Usually, each gully has an alcove, channel, and apron.[9] [10] [11] For years, many believed that gullies were formed by running water, but further observations demonstrate that they may be formed by dry ice.[12] [13] [14] In some years frost, perhaps as thick as 1 meter, triggers avalanches. This frost contains mostly dry ice, but also has tiny amounts of water ice.[15]


  • Chincoteague Crater

  • Close-up of Chincoteague Crater, as seen by HiRISE Gullies are visible. Gullies may be created by water and/or dry ice moving down the crater walls. The exact cause is debatable at present.

Pedestal craters

A pedestal crater is an impact crater which has its ejecta sitting above the surrounding terrain. This forms a raised platform (like a pedestal). These craters are produced when an impact crater ejects material that forms an erosion-resistant layer at the top, thus causing the immediate area to erode more slowly than the rest of the region. Some pedestals have been accurately measured to be hundreds of meters above the surrounding area. This means that hundreds of meters of material were eroded away. The result is that both the crater and its ejecta blanket stand above the surroundings. Pedestal craters were first observed during the Mariner missions.[16] [17] [18] [19] Much of the material under the pedestal crater’ ejecta may be ice. These types of craters may be useful for finding sources of water ice since they can be easily spotted and mapped from orbit.

  • Pedestal crater

  • Pedestal crater

Channels

There is enormous evidence that water once flowed in river valleys on Mars.[20] [21] Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the Mariner 9 orbiter.[22] [23] [24] [25] In fact, a study published in June 2017, estimated 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.[26] [27]

  • Hrad Vallis, as seen by CTX Photo labeled with layers, streamlined forms, and arrow indicating direction water flowed.

  • Channel, as seen by HiRISE under HiWish program

Volcano-ice interactions

Large amounts of water ice are believed to be present just under the surface of Mars. Some channels lie near volcanic areas. When hot subsurface magma comes close to this ice, large amounts of liquid water and mud may be formed. Hrad Vallis in the Cebrenia quadrangle is close to the large volcano, Elysium Mons. It may have supplied heat to melt ice and make the channel. Hrad Vallis is pictured below.[28]

  • Hrad Vallis may have been formed when the large Elysium Mons volcanic complex melted ground ice, as seen by THEMIS.

  • Streamlined islands in Hrad Vallis, as seen by HiRISE.

Layered structures

Some locations on Mars display layered features in craters, depressions, and leaning on mesas. These are probably the remains of materials that once covered a wide region. They may mostly consist of latitude dependent mantle which falls from the sky as ice-rich particles.


Wide view of groups of layers, as seen by HiRISE under HiWish program These layers probably represent mantle deposited when climate changed. They were shaped by the wind.


Close view of a group of layers program Note: This is an enlargement from the previous image.

Latitude dependent mantle

Mantle may be composed of ice and dust that fell from the sky during past climatic conditions. Mantle could be a major source of water for future colonists because it is fairly common and could be mined for water by robotic machines.

Close up view of mantle, as seen by HiRISE under the HiWish program. Mantle may be composed of ice and dust that fell from the sky during past climatic conditions.


Latitude dependent mantle

Glaciers

Since the 60’s, as our spacecraft have studied Mars with more and more advanced cameras and other instruments, we have found more and more evidence for glaciers. [29] [30] [31] [32] [33] [34] [35] On Mars these glaciers are covered with rock and dust debris a few meters to a few tens of meters thick. Even though Mars today is too dry for any glaciers, this covering material has protected the underlying ice. [36] One would think that under today’s conditions any exposed ice would undergo sublimation and disappear into the thin Martian atmosphere. That is, it would go directly from a solid to a gas. However, the insulating effect of surface debris prevents the loss of ice.[33] [36] [37] [38][39][40]

Wide view of a cliff and remains of a glacier, as seen by HiRISE

Lobate Debris Aprons

Features, called lobate debris aprons (LDA’s), around mesas are actually now accepted to be glaciers. These LDA’s looked like glaciers; final proof came with radar studies. The Shallow Subsurface Radar (SHARD) on board the Mars Reconnaissance Orbiter discovered that lobate debris aprons (LDA’s), around mesas were mostly ice under a thin rock debris cover. [41] [42] Ice was found both in the southern and northern hemispheres. [43] [44] [45]


Lobate debris apron in Phlegra Montes, as seen by HiRISE. The debris apron is probably mostly ice with a thin covering of rock debris, so it could be a source of water for future Martian colonists. Scale bar is 500 meters long.

Lineated Valley Fill

Close view of lineated valley fill on left and mantle on right, as seen by HiRISE under HiWish program

Close view of lineated valley fill on left and mantle on right, as seen by HiRISE under HiWish program


Another ice-rich feature is called lineated valley fill (LVF). [46] [47] [48] It covers many of the wide, flat valley floors of fretted terrain. LVF may have formed from the interaction of glaciers coming out of valleys and from mesas eroding, it has similar surface appearance of other supposed glaciers, including LDA. The surface resembles the human brain. Since the material covering ice is shaped into something resembling the human brain, it is named brain terrain. Brain terrain starts to form with cracks in the ice-rich surface. Sublimation along the cracks turns the cracks into small valleys. [49] [50] [51] [52] [53] [54] [55]

Brain terrain on crater floor, as seen by HiRISE under HiWish program Brain terrain forms when cracks form and get larger.


Close view of lineated valley fill on left and mantle on right, as seen by HiRISE under HiWish program

Chaos

Galaxias Chaos, as seen by CTX.


This series of drawings shows a model for the formation of Martian chaos, as proposed by Pedersen and Head 2011[56] Amount of sublimation is exaggerated to improve understanding. Click on image to see more details.


Some areas of Mars are classified as regions of “Chaos.” The ground seems to have collapsed. Often large blocks and hills are present in abundance. Many have large outflow channels associated with them. Galaxias Chaos in the Cebrenia quadrangle is different from most other chaotic regions. It does not have outflow channels, and it does not show a great elevation difference between it and the neighboring land area. Research by Pedersen and Head, published in 2010, suggests that Galaxias Chaos is the site of a volcanic flow that buried an ice-rich layer. That buried layer is a residue from water-rich materials deposited by large floods.[57] [58] Since the upper lava cap would not be supported evenly all over, it would crack. Along the cracks sublimation of water into the thin Martian atmosphere would be more intense. A blocky terrain that is typical of chaos would eventually develop. The sublimation process may have been facilitated by heat from magma movements. There are volcanoes, namely Elysium Montes and Hecates Tholus, close by which probably are surrounded by dikes, which would have heated the ground. Dikes occur when magma goes into cracks and weak areas rather than to the top of a volcano. They are widespread around most volcanoes. Shiprock, New Mexico contains typical dikes that have been exposed by erosion. Also, a warmer period in the past would have increased the amount of water sublimating from the ground.[59]

Ice exposed in new craters

Ice in crater Location: 43.286° N and 164.213°E Two pictures from HiRISE showing how ice disappeared over time in a crater. Crater on left is before ice disappeared. Crater is 6 meters in diameter.

Remarkable research, published in the journal Science in September 2009.[60] reported that some new craters on Mars show exposed, pure, water ice. Furthermore, scientists watched the ice disappear, presumably evaporating into the atmosphere by the process of sublimation. The ice is only a few feet deep. The Compact Imaging Spectrometer (CRISM)] on board the Mars Reconnaissance Orbiter (MRO ) confirmed that the bright substance was indeed water ice. The ice was found in a total of 5 locations. Three of the locations are in the Cebrenia quadrangle. These locations are 55.57 N 150.62 E (209.38 W), 43.28 N 176.9 E (183.1 W), and 45 N 164.5 E (195.5 W).[61] [62] [63] [64] This discovery proves that future colonists on Mars will be able to obtain water from a wide variety of locations. This ice can be dug up, melted, and then taken apart to provide fresh oxygen and hydrogen for rocket fuel. Hydrogen is the powerful fuel used by the space shuttle main engines. Robotic machines may be invented to mine and bring ice to future colonies.

Cones

  • Cones Some cones are thought to be mud volcanoes. Since the mud has been brought up from some depth it may contain remains of life that were protected from radiation at the surface.

Viking’s Findings

Viking 2’s lander at about 200 km west of Mie Crater in Utopia Planitia at 47.64 degrees N and 134.29 degrees E (225.71 W).[65] The location can easily be seen on maps of Mars because Mie Crater sits by itself. For over four years it imaged the surface, analyzed soil samples, and performed experiments that looked for life. The last message from Viking Lander 2 came to Earth on April 11,1980.[66] The last communication with the Viking 2 Orbiter occurred on July 25, 1978.[67] By the end of the Orbiter’s mission, it had returned nearly 16,000 images in its 706 orbits around the Red Planet.[68]

View of surface around Viking 2 

                                                          View of surface around Viking 2

Minerals detected in the soil were similar to those produced from the weathering of basaltic lavas on Earth. Dirt at this site contained abundant silicon and iron, in addition to significant amounts of magnesium, aluminum, sulfur, calcium, and titanium. Strontium and yttrium were found in trace amounts. Potassium was 5 times lower than the average in the Earth's crust. Sulfur and chlorine were similar to compounds that remain after sea water evaporates. Sulfur was more concentrated in the top crust of the soil than in the underlying bulk soil. Sulfur could be in the form of sulfates of sodium, magnesium, calcium, or iron. Iron sulfide is also possible. [69]

Elements in the soil were found with an X-ray fluorescence spectrometer.[70] Mineral models suggest that the soil could be a mixture of about 90% iron-rich clay, about 10% magnesium sulfate (kieserite?), about 5% carbonate (calcite), and about 5% iron oxides (hematite, magnetite, goethite?). These minerals are typical weathering products of mafic igneous rocks.

The dark, igneous rock basalt is believed to make up much of the surface of Mars, as it does for the Earth.[71] [72] [73]

Studies with magnets aboard the Viking landers indicated that the soil is between 3 and 7 percent magnetic materials by weight. The magnetic chemicals could be magnetite and maghemite. These could come from the weathering of basalt rock.[74] [75]

Map showing locations of Viking landers and Pathfinder Note Viking 2 in far North. 

    Map showing locations of Viking landers and Pathfinder  Note Viking 2 in far North.

Viking 2 gathered weather data for over 4 years while active on the surface. Temperatures at this location varied from a low of -189.4 degrees F (-123 C, 150 K) to a high of -9.4 degrees F (-23 C, 250 K). As these temperatures were recorded in the far north, cold temperatures would be expected. Furthermore, pressure changes, seasonal dust storms, and transport of atmospheric gases between the polar caps were observed.[76] Three experiments on Viking looked for life. Granted that some activity was observed, most scientists now believe that the data came from inorganic chemical reactions of the soil. Nevertheless, a few scientists still to this day believe the results were due to living organisms.[77] [78] [79] Because no organic chemicals were found in the soil, most scientists concluded there was no life detected at this location. However, dry areas of Antarctica do not have detectable organic compounds either, but they have organisms living in the rocks.[80]

Early on, some scientists suggested that the lack of a protective ozone layer would cause UV light to sterilize the soil surface. Mars has almost no ozone layer, so UV light sanitizes the surface and may produce peroxides that would change any organic chemicals.[81] These theories did seem to be validated, decades later when the Phoenix Lander detected the chemical perchlorate in the Martian Soil. Perchlorate, a strong oxidant, may have wiped out all traces of organic matter in the Martian soil.[82] Carbon-based life would be difficult at the soil surface, if perchlorates were pervasive on Mars. In addition, a study published in the Journal of Geophysical Research in 2010, suggested that organic compounds were actually present in the soil analyzed by both Viking 1 and 2. The study's authors discovered that perchlorate will destroy organics when heated and will produce chloromethane and dichloromethane--the same chlorine compounds discovered by both Viking landers when they performed the tests on Mars. [83] [84] [85] [86]Since perchlorate would have broken down any Martian organics, there could be life at the Viking sites.[87] [88]

References

  1. ↑ 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.
  2. ↑ 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.
  3. ↑ http://planetarynames.wr.usgs.gov/Feature/1095
  4. ↑ https://planetarynames.wr.usgs.gov/
  5. ↑ https://en.wikipedia.org/wiki/Cebrenia_quadrangle#Physiography_and_geology
  6. ↑ Ezell E. K., Ezell L. N. On Mars: Exploration of the Red Planet. 1958-1978. (Chapter 10). The NASA History Series. Scientific and Technical Information Branch, 1984. NASA, Washington, D.C.
  7. ↑ Hugh H. Kieffer (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7.
  8. ↑ Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ%7Caccessdate=7 March 2011|year=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7
  9. ↑ Edgett |first1= K. |last2= Malin |first2= M. C. |last3= Williams |first3= R. M. E. |last4= Davis |first4= S. D. |date= 2003 |title= Polar-and middle-latitude martian gullies: A view from MGS MOC after 2 Mars years in the mapping orbit |journal= Lunar Planet. Sci. |volume=34 |at=p. 1038, Abstract 1038 | url=http://www.lpi.usra.edu/meetings/lpsc2003/pdf/1038.pdf |
  10. ↑ Dickson | first1 = J | last2 = Head | first2 = J | last3 = Kreslavsky | first3 = M | title = Martian gullies in the southern mid-latitudes of Mars: Evidence for climate-controlled formation of young fluvial features based upon local and global topography | doi = 10.1016/j.icarus.2006.11.020 |
  11. ↑ http://www.planetary.brown.edu/pdfs/3138.pdf | date = 2007 | pages = 315–323 | volume = 188 | issue = 2 | journal = Icarus |
  12. ↑ http://www.jpl.nasa.gov/news/news.php?release=2014-226
  13. ↑ http://hirise.lpl.arizona.edu/ESP_032078_1420
  14. ↑ http://www.space.com/26534-mars-gullies-dry-ice.html
  15. ↑ http://spaceref.com/mars/frosty-gullies-on-mars.html
  16. ↑ http://hirise.lpl.eduPSP_008508_1870
  17. ↑ Bleacher, J. and S. Sakimoto. Pedestal Craters, A Tool For Interpreting Geological Histories and Estimating Erosion Rates. LPSC
  18. ↑ http://themis.asu.edu/feature_utopiacraters
  19. ↑ McCauley, John F. (December 1972). "Mariner 9 Evidence for Wind Erosion in the Equatorial and Mid-Latitude Regions of Mars". Journal of Geophysical Research. 78 (20): 4123–4137(JGRHomepage).
  20. ↑ Baker, V., et al. 2015. Fluvial geomorphology on Earth-like planetary surfaces: a review. Geomorphology. 245, 149–182.
  21. ↑ Carr, M. 1996. in Water on Mars. Oxford Univ. Press.
  22. ↑ Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX
  23. ↑ 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.
  24. ↑ Carr, M. 1979. Formation of Martian flood features by release of water from confined aquifers. J. Geophys. Res. 84, 2995–300.
  25. ↑ 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.
  26. ↑ http://spaceref.com/mars/how-much-water-was-needed-to-carve-valleys-on-mars.html
  27. ↑ 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
  28. ↑ http://themis.asu.edu/zoom-20020715a.html
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  38. ↑ Head, J., et al. 2009. Northern mid-latitude glaciation in the Late Amazonian period of Mars: Criteria for the recognition of debris-covered glacier and valley glacier landsystem deposits. Earth and Planetary Science Letters. Doi:10.1016/j.epsl.2009.06.041
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  40. ↑ Hubbard, Bryn, et al. "Geomorphological characterization and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars." Icarus 211.1 (2011): 330-346.
  41. ↑ Plaut, J. et al. 2008. Radar Evidence for Ice in Lobate Debris Aprons in the Mid-Northern Latitudes of Mars. Lunar and Planetary Science XXXIX. 2290.pdf
  42. ↑ http://hirise.lpl.arizona.edu/PSP_009535_2240
  43. ↑ cite journal | last1 = Holt | first1 = J. | last2 = Safaeinili | first2 = A. | last3 = Plaut | first3 = J. | last4 = Head | first4 = J. | last5 = Phillips | first5 = R. | last6 = Seu | first6 = R. | last7 = Kempf | first7 = S. | last8 = Choudhary | first8 = P. | last9 = Young | first9 = D. | last10 = Putzig | first10 = N. | last11 = Biccari | first11 = D. | last12 = Gim | first12 = Y. | year = 2008 | title = Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars | url = | journal = Science | volume = 322| issue = | pages = 1235–1238| doi = 10.1126/science.1164246 | pmid=19023078|
  44. ↑ cite journal | last1 = Plaut | first1 = J. | last2 = Safaeinili | first2 = A. | last3 = Holt | first3 = J. | last4 = Phillips | first4 = R. | last5 = Head | first5 = J. | last6 = Seu | first6 = R. | last7 = Putzig | first7 = N. | last8 = Frigeri | first8 = A. | year = 2009 | title = Radar evidence for ice in lobate debris aprons in the midnorthern latitudes of Mars | url = | journal = Geophys. Res. Lett. | volume = 36| issue = | page = | doi = 10.1029/2008GL036379 |
  45. ↑ Holt, J., et al. 2008. Radar Sounding Evidence for Ice within Lobate Debris Aprons, near Hellas Basin, Mid-southern Latitudes of Mars. Lunar and Planetary Science XXXIX. 2441.pdf
  46. ↑ Carr, M. 2006. The Surface of Mars. Cambridge University Press. ISBN|978-0-521-87201-0
  47. ↑ Squyres, S. 1978. Martian fretted terrain: Flow of erosional debris. Icarus: 34. 600-613.
  48. ↑ Levy. et al. 2007. Lineated valley fill and lobate debris apron stratigraphy in Nilosyrtis Mensae, Mars: Evidence for phases of glacial modification of the dichotomy boundary. J. Geophys. Res. 112
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  50. ↑ Levy, J. et al. 2009. Concentric crater fill in Utopia Planitia: History and interaction between glacial "brain terrain" and periglacial processes. Icarus: 202. 462-476.
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  52. ↑ cite journal |author1=Head, J. |author2=D. Marchant |lastauthoramp=yes| date = 2006 | title = Modification of the walls of a Noachian crater in northern Arabia Terra (24E, 39N) during mid-latitude Amazonian glacial epochs on Mars: Nature and evolution of lobate debris aprons and their relationships to lineated valley fill and glacial systems | journal = Lunar Planet. Sci | volume = 37 | page = Abstract # 1126
  53. ↑ cite journal | author = Kress, A., J. Head | date = 2008 | title = Ring-mold craters in lineated valley fill and lobate debris aprons on Mars: Evidence for subsurface glacial ice | journal = Geophys. Res. Lett. | volume = 35 | page = L23206–8 | doi=10.1029/2008gl035501|
  54. ↑ cite journal | author = Baker, D. | date = 2010 | title = Flow patterns of lobate debris aprons and lineated valley fill north of Ismeniae Fossae, Mars: Evidence for extensive mid-latitude glaciation in the Late Amazonian | journal = Icarus | volume = 207 | pages = 186–209 | doi = 10.1016/j.icarus.2009.11.017 | last2 = Head | first2 = James W. | last3 = Marchant | first3 = David R.
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See Also

Recommended reading

  • Grotzinger, J., R. Milliken (eds.). 2012. Sedimentary Geology of Mars. Tulsa: Society for Sedimentary Geology.
  • Kieffer, H., et al. (eds) 1992. Mars. The University of Arizona Press. Tucson
  • September 30, 1977 issue of the Journal of Geophysical Research, "Scientific Results of the Viking Project", vol. 82, no. 28.
  • history.nasa.gov/SP-4212/ch11

External links


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