https://marspedia.org/index.php?title=Cebrenia_quadrangle&feed=atom&action=historyCebrenia quadrangle - Revision history2024-03-28T18:50:17ZRevision history for this page on the wikiMediaWiki 1.34.2https://marspedia.org/index.php?title=Cebrenia_quadrangle&diff=136537&oldid=prevSuitupandshowup: /* External links */ added link2020-11-03T23:15:13Z<p><span dir="auto"><span class="autocomment">External links: </span> added link</span></p>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*https://www.youtube.com/watch?v=CoMbVt7qdH8 Mars Clips 15 The Cebrenia Region Viking 2 Lander video </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>*https://www.youtube.com/watch?v=CoMbVt7qdH8 Mars Clips 15 The Cebrenia Region Viking 2 Lander video </div></td></tr>
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</table>Suitupandshowuphttps://marspedia.org/index.php?title=Cebrenia_quadrangle&diff=135518&oldid=prevSuitupandshowup at 18:40, 29 March 20202020-03-29T18:40:59Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Image:MOLA hecates tholus.jpg |thumb|300px|center| Tographic map of area around Hecates Tholus]]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Image:MOLA hecates tholus.jpg |thumb|300px|center| Tographic map of area around Hecates Tholus]]</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div> [[Image:27108hecatechannels.jpg |thumb|right|300px|Lava channels on Hecates Tholus]]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div> [[Image:27108hecatechannels.jpg |thumb|right|300px|Lava channels on Hecates Tholus]]</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Craters==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Craters==</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.<ref <del class="diffchange diffchange-inline">name="Kieffer1992"</del>><del class="diffchange diffchange-inline">{{cite book|author=</del>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<del class="diffchange diffchange-inline">}}</del></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.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div> </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" widths="380px" heights="360px"></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" widths="380px" heights="360px"></div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Layered structures==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Layered structures==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Some locations on Mars display layered features in craters, depressions, and <del class="diffchange diffchange-inline">next to </del>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.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Some locations on Mars display layered features in craters, depressions, and <ins class="diffchange diffchange-inline"> leaning on </ins>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.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>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. <del class="diffchange diffchange-inline">Probably </del>formed from the interaction of glaciers coming out of valleys and <del class="diffchange diffchange-inline">of </del>mesas eroding, it has similar surface appearance of other supposed glaciers, including LDA. <del class="diffchange diffchange-inline">It looks like </del>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></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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. <ins class="diffchange diffchange-inline">LVF may have </ins>formed from the interaction of glaciers coming out of valleys and <ins class="diffchange diffchange-inline">from </ins>mesas eroding, it has similar surface appearance of other supposed glaciers, including LDA. <ins class="diffchange diffchange-inline">The surface resembles </ins>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></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.]]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[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.]]</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>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. <del class="diffchange diffchange-inline">Ship rock</del>, 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></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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. <ins class="diffchange diffchange-inline">Shiprock</ins>, 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></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Ice exposed in new craters==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Ice exposed in new craters==</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div> View of surface around Viking 2</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div> View of surface around Viking 2</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>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> <del class="diffchange diffchange-inline"> </del>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></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div> </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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. </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div> </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div> </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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> </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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> </div></td></tr>
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</table>Suitupandshowuphttps://marspedia.org/index.php?title=Cebrenia_quadrangle&diff=135517&oldid=prevSuitupandshowup: /* Gullies */ added info and ref2020-03-29T18:28:52Z<p><span dir="auto"><span class="autocomment">Gullies: </span> added info and ref</span></p>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Gullies==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Gullies==</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">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></ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">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></ins></div></td></tr>
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</table>Suitupandshowuphttps://marspedia.org/index.php?title=Cebrenia_quadrangle&diff=135516&oldid=prevSuitupandshowup at 18:26, 29 March 20202020-03-29T18:26:12Z<p></p>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div></gallery></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div></gallery></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>This article aims to describe the <del class="diffchange diffchange-inline">location and </del>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.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div> </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div> </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Origin of name==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Origin of name==</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l21" >Line 21:</td>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Viking 2 landed near <del class="diffchange diffchange-inline">MieCrater </del>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></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Viking 2 landed near <ins class="diffchange diffchange-inline">Mie Crater </ins>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></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==[[Hecates Tholus]]==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==[[Hecates Tholus]]==</div></td></tr>
</table>Suitupandshowuphttps://marspedia.org/index.php?title=Cebrenia_quadrangle&diff=135289&oldid=prevSuitupandshowup at 15:15, 21 March 20202020-03-21T15:15:28Z<p></p>
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<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 15:15, 21 March 2020</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l32" >Line 32:</td>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" widths="<del class="diffchange diffchange-inline">190px</del>" heights="<del class="diffchange diffchange-inline">180px</del>"></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" <ins class="diffchange diffchange-inline"> </ins>widths="<ins class="diffchange diffchange-inline">380px</ins>" heights="<ins class="diffchange diffchange-inline">360px</ins>"></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:ESP 056607 2170layers.jpg|Crater showing layers, as seen by HiRISE under HiWish program</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:ESP 056607 2170layers.jpg|Crater showing layers, as seen by HiRISE under HiWish program</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Gullies==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Gullies==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" widths="<del class="diffchange diffchange-inline">190px</del>" heights="<del class="diffchange diffchange-inline">180px</del>"></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" <ins class="diffchange diffchange-inline"> </ins>widths="<ins class="diffchange diffchange-inline">380px</ins>" heights="<ins class="diffchange diffchange-inline">360px</ins>"></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:Chincoteague Crater.jpg|Chincoteague Crater</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:Chincoteague Crater.jpg|Chincoteague Crater</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td></tr>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" widths="<del class="diffchange diffchange-inline">190px</del>" heights="<del class="diffchange diffchange-inline">180px</del>"></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div> </div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" <ins class="diffchange diffchange-inline"> </ins>widths="<ins class="diffchange diffchange-inline">380px</ins>" heights="<ins class="diffchange diffchange-inline">360px</ins>"></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:ESP 047772 2210pedestal.jpg|Pedestal crater </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:ESP 047772 2210pedestal.jpg|Pedestal crater </div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:ESP 048021 2130pedestal.jpg|Pedestal crater</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:ESP 048021 2130pedestal.jpg|Pedestal crater</div></td></tr>
<tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l62" >Line 62:</td>
<td colspan="2" class="diff-lineno">Line 63:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" widths="<del class="diffchange diffchange-inline">190px</del>" heights="<del class="diffchange diffchange-inline">180px</del>"></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" <ins class="diffchange diffchange-inline"> </ins>widths="<ins class="diffchange diffchange-inline">380px</ins>" heights="<ins class="diffchange diffchange-inline">360px</ins>"></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:47653 2150ctxchannel.jpg| Hrad Vallis, as seen by CTX Photo labeled with layers, streamlined forms, and arrow indicating direction water flowed.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:47653 2150ctxchannel.jpg| Hrad Vallis, as seen by CTX Photo labeled with layers, streamlined forms, and arrow indicating direction water flowed.</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:ESP 052738 2135channel.jpg|Channel, as seen by HiRISE under HiWish program</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:ESP 052738 2135channel.jpg|Channel, as seen by HiRISE under HiWish program</div></td></tr>
<tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l71" >Line 71:</td>
<td colspan="2" class="diff-lineno">Line 72:</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" widths="<del class="diffchange diffchange-inline">190px</del>" heights="<del class="diffchange diffchange-inline">180px</del>"></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" <ins class="diffchange diffchange-inline"> </ins>widths="<ins class="diffchange diffchange-inline">380px</ins>" heights="<ins class="diffchange diffchange-inline">360px</ins>"></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td></tr>
<tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l146" >Line 146:</td>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Cones==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Cones==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" widths="<del class="diffchange diffchange-inline">190px</del>" heights="<del class="diffchange diffchange-inline">180px</del>"></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><gallery class="center" <ins class="diffchange diffchange-inline"> </ins>widths="<ins class="diffchange diffchange-inline">380px</ins>" heights="<ins class="diffchange diffchange-inline">360px</ins>"></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>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.</div></td></tr>
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</table>Suitupandshowuphttps://marspedia.org/index.php?title=Cebrenia_quadrangle&diff=132743&oldid=prevMichel Lamontagne at 14:11, 21 January 20202020-01-21T14:11:00Z<p></p>
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</table>Michel Lamontagnehttps://marspedia.org/index.php?title=Cebrenia_quadrangle&diff=132626&oldid=prevMichel Lamontagne at 20:05, 18 January 20202020-01-18T20:05:57Z<p></p>
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<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><gallery widths="400" heights="<del class="diffchange diffchange-inline">400</del>"></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><gallery widths="400" heights="<ins class="diffchange diffchange-inline">300</ins>"></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:USGS-Mars-MC-7-CebreniaRegion-mola.png</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:USGS-Mars-MC-7-CebreniaRegion-mola.png</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:PIA00167-MC-7-CebreniaRegion-19980605.jpg|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).</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>File:PIA00167-MC-7-CebreniaRegion-19980605.jpg|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).</div></td></tr>
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</table>Michel Lamontagnehttps://marspedia.org/index.php?title=Cebrenia_quadrangle&diff=132625&oldid=prevMichel Lamontagne at 20:05, 18 January 20202020-01-18T20:05:25Z<p></p>
<a href="//marspedia.org/index.php?title=Cebrenia_quadrangle&diff=132625&oldid=132525">Show changes</a>Michel Lamontagnehttps://marspedia.org/index.php?title=Cebrenia_quadrangle&diff=132525&oldid=prevMichel Lamontagne at 02:36, 9 January 20202020-01-09T02:36:32Z<p></p>
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<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 02:36, 9 January 2020</td>
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<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>{| class="wikitable sortable"</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>{| class="wikitable sortable"</div></td></tr>
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</table>Michel Lamontagnehttps://marspedia.org/index.php?title=Cebrenia_quadrangle&diff=132413&oldid=prevMichel Lamontagne at 23:03, 7 January 20202020-01-07T23:03:28Z<p></p>
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<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|MC-<del class="diffchange diffchange-inline">30</del></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|MC-<ins class="diffchange diffchange-inline">07</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|Cebrenia quadrangle</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|Cebrenia quadrangle</div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|<del class="diffchange diffchange-inline">65–90° S</del></div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|<ins class="diffchange diffchange-inline">30–65° N</ins></div></td></tr>
<tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>|<del class="diffchange diffchange-inline">180° W – 180° </del>E</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>|<ins class="diffchange diffchange-inline">120°–180° </ins>E</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|[[Mars Quadrangles|Quadrangles]]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|[[Mars Quadrangles|Quadrangles]]</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|[[Mars atlas|Atlas]]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|[[Mars atlas|Atlas]]</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|}</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|}</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[File:PIA00167-MC-7-CebreniaRegion-19980605.jpg|thumb|400px|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).]]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[File:PIA00167-MC-7-CebreniaRegion-19980605.jpg|thumb|400px|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).]]</div></td></tr>
</table>Michel Lamontagne