http://marspedia.org/api.php?hidebots=1&urlversion=1&days=7&limit=50&target=Mars_Atlas&action=feedrecentchanges&feedformat=atomMarspedia - Changes related to "Mars Atlas" [en]2024-03-29T09:41:10ZRelated changesMediaWiki 1.34.2http://marspedia.org/index.php?title=Phoenicis_Lacus_quadrangle&diff=140927&oldid=140625Phoenicis Lacus quadrangle2024-03-28T15:44:22Z<p>added new info and ref</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>The most common form of volcanism on the Earth is basaltic. Basalts formed from molten rocks that cooled on the surface. They originated from the partial melting of the upper mantle. They are rich in the elements iron and magnesium (so they are classified as mafic minerals) and are commonly dark gray in color. The principal type of volcanism on Mars is probably also basaltic.<ref>Carr | first1=Michael H. | publisher=Cambridge University Press | isbn= 978-0-521-87201-0 | title= The Surface of Mars |year=2006 | ref =harv | location=New York</ref> Although Mars displays numerous volcanoes here and in other places, there has been no evidence of recent volcanic activity, even at a very low level. Research, from 2017, found no active release of volcanic gases during two successive Martian years. The research team looked for the outgassing of sulfur-bearing chemicals with spectrometers.<ref>Khayat, A., et al. 2017. A deep search for the release of volcanic gases on Mars using ground-based high-resolution infrared and submillimeter spectroscopy: Sensitive upper limits for OCS and SO2. Icarus: 296, 1-14.</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 most common form of volcanism on the Earth is basaltic. Basalts formed from molten rocks that cooled on the surface. They originated from the partial melting of the upper mantle. They are rich in the elements iron and magnesium (so they are classified as mafic minerals) and are commonly dark gray in color. The principal type of volcanism on Mars is probably also basaltic.<ref>Carr | first1=Michael H. | publisher=Cambridge University Press | isbn= 978-0-521-87201-0 | title= The Surface of Mars |year=2006 | ref =harv | location=New York</ref> Although Mars displays numerous volcanoes here and in other places, there has been no evidence of recent volcanic activity, even at a very low level. Research, from 2017, found no active release of volcanic gases during two successive Martian years. The research team looked for the outgassing of sulfur-bearing chemicals with spectrometers.<ref>Khayat, A., et al. 2017. A deep search for the release of volcanic gases on Mars using ground-based high-resolution infrared and submillimeter spectroscopy: Sensitive upper limits for OCS and SO2. Icarus: 296, 1-14.</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><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;">The dsovery of a new volcano at the east side of Noctis Labrinthus was announced at a conference in March 2024. It was seen since the early 1970s, but erosion had concealed it from view. </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;">The new volcano has a diameter of about 280 miles (450 kilometers and measures roughly 29,600 feet (9,022 meters) in elevation. Note: this mountain is higher than any peak in the United States. Lava flows, pyroclastic deposits (made of volcanic materials such as ash, cinders, pumice and tephra) and hydrothermal mineral deposits occur in several areas nearby.<ref>https://www.space.com/mars-giant-volcano-hiding-plain-sight?utm_term=CABA215D-3D47-4C9A-92FE-9ECF8D4C7909&lrh=e62336263a3610a07ef7c8af2080c758f2ecd0661aab1a8e6234cf31f0d0fdff&utm_campaign=58E4DE65-C57F-4CD3-9A5A-609994E2C5A9&utm_medium=email&utm_content=DBDE44BA-0009-4913-99AB-1A1AD0DC4FF9&utm_source=SmartBrief</ref> The volcano is located at 7.40°S, 94.60°W. The authors of the paper consider the volcano to be an eroded shield</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;">volcano. Sub-circular depressions near the top are interpreted as caldera remnants.<ref>https://www.hou.usra.edu/meetings/lpsc2024/pdf/2745.pdf</ref></ins></div></td></tr>
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</table>Suitupshowuphttp://marspedia.org/index.php?title=Ismenius_Lacus_quadrangle&diff=140926&oldid=140915Ismenius Lacus quadrangle2024-03-28T13:01:05Z<p></p>
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</tr><tr><td colspan="4" class="diff-multi" lang="en">(3 intermediate revisions by the same user not shown)</td></tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l461" >Line 461:</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>==Dipping layers==</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>==Dipping layers==</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>Scattered around Mars are features that have been called "dipping layers" <del class="diffchange diffchange-inline"> </del>They are groups of layers in protected place like inside of craters or against slopes. <del class="diffchange diffchange-inline">They once covered a wide area</del>, <del class="diffchange diffchange-inline">but erosion has since removed most of the material</del>. The material that formed them may <del class="diffchange diffchange-inline">fell </del>from the sky as ice-rich dust.<ref>Carr, M. 2001. Mars Global Surveyor observations of martian fretted terrain. J. Geophys. Res. 106, 23571-23593.</ref> <ref>Baker, D., J. Head. 2015. Extensive Middle Amazonian mantling of debris aprons and plains in Deuteronilus Mensae, Mars: Implication for the record of mid-latitude glaciation. Icarus: 260, 269-288</ref> <del class="diffchange diffchange-inline"> </del>Another idea for their origin was presented at 55th LPSC (2024) by an international team of researchers. They suggest that the layers are from past ice sheets.<ref>Blanc, E., et al. 2024. ORIGIN OF WIDESPREAD LAYERED DEPOSITS ASSOCIATED WITH MARTIAN DEBRIS COVERED GLACIERS. 55th LPSC (2024). 1466.pdf</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>Scattered around Mars are features that have been called "dipping layers<ins class="diffchange diffchange-inline">.</ins>" They are groups of layers in protected place like inside of craters or against slopes. <ins class="diffchange diffchange-inline">Several ideas have been advanced for how they were formed.<ref> R.J. Soare et al. 2013. Sub-kilometre (intra-crater) mounds in Utopia Planitia, Mars: character, occurrence and possible formation hypotheses, Icarus, 225</ins>, <ins class="diffchange diffchange-inline">982–991</ins>.<ins class="diffchange diffchange-inline"></ref> </ins> The material that formed them may <ins class="diffchange diffchange-inline">have dropped </ins>from the sky as ice-rich dust.<ins class="diffchange diffchange-inline"><ref>Morgenstern, A,, et al. 2007. Deposition and degradation of a volatile-rich layer in Utopia Planitia and implications for climate history on Mars. Journal of Geophysical Research Planets. Volume 112. IssueE6</ref> </ins><ref>Carr, M. 2001. <ins class="diffchange diffchange-inline">"</ins>Mars Global Surveyor observations of martian fretted terrain<ins class="diffchange diffchange-inline">"</ins>. <ins class="diffchange diffchange-inline">''</ins>J. Geophys. Res.<ins class="diffchange diffchange-inline">'' </ins>106, 23571-23593.</ref> <ref>Baker, D., J. Head. 2015. <ins class="diffchange diffchange-inline">"</ins>Extensive Middle Amazonian mantling of debris aprons and plains in Deuteronilus Mensae, Mars: Implication for the record of mid-latitude glaciation<ins class="diffchange diffchange-inline">"</ins>. <ins class="diffchange diffchange-inline">''</ins>Icarus<ins class="diffchange diffchange-inline">''</ins>: 260, 269-288</ref> <ins class="diffchange diffchange-inline">They once covered a wide area, but erosion has since removed most of the material. </ins>Another idea for their origin was presented at 55th LPSC (2024) by an international team of researchers. They suggest that the layers are from past ice sheets.<ref>Blanc, E., et al. 2024. ORIGIN OF WIDESPREAD LAYERED DEPOSITS ASSOCIATED WITH MARTIAN DEBRIS COVERED GLACIERS. 55th LPSC (2024). 1466.pdf</ref> </div></td></tr>
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</table>Suitupshowuphttp://marspedia.org/index.php?title=Diacria_quadrangle&diff=140922&oldid=140653Diacria quadrangle2024-03-27T21:50:09Z<p><span dir="auto"><span class="autocomment">Ice exposed in new craters: </span> added image</span></p>
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<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 21:50, 27 March 2024</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>A study reported in the journal Science in 2009 shows that some newly formed craters have excavated clean, water ice from just below the surface in five locations on Mars. <ref>Byrne, S. et al. 2009. Distribution of Mid-Latitude Ground Ice on Mars from New Impact Craters: 329.1674-1676</ref> After a short time, the ice disappears, subliming into the atmosphere. The ice is only a few meters deep. The ice was confirmed with the Compact Imaging Spectrometer (CRISM) on board the [[Mars Reconnaissance Orbiter]] (MRO). The ice was found in a total of 5 locations. One of the locations (Site 5) is in the Diacria quadrangle at about 46° N, 182° E (178 W).<ref>http://www.space.com/scienceastronomy/090924-mars-crater-ice.html</ref><ref>http://news.aol.com/article/nasa-spacecraft-sees-ice-on-mars-exposed/686020</ref> <ref>http://nasa.gov/mission/MRO/news/mro20090924.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>A study reported in the journal Science in 2009 shows that some newly formed craters have excavated clean, water ice from just below the surface in five locations on Mars. <ref>Byrne, S. et al. 2009. Distribution of Mid-Latitude Ground Ice on Mars from New Impact Craters: 329.1674-1676</ref> After a short time, the ice disappears, subliming into the atmosphere. The ice is only a few meters deep. The ice was confirmed with the Compact Imaging Spectrometer (CRISM) on board the [[Mars Reconnaissance Orbiter]] (MRO). The ice was found in a total of 5 locations. One of the locations (Site 5) is in the Diacria quadrangle at about 46° N, 182° E (178 W).<ref>http://www.space.com/scienceastronomy/090924-mars-crater-ice.html</ref><ref>http://news.aol.com/article/nasa-spacecraft-sees-ice-on-mars-exposed/686020</ref> <ref>http://nasa.gov/mission/MRO/news/mro20090924.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;"><div>This discovery is significant because it shows the presence of subsurface ice at latitudes further south than expected and proves that future colonists on Mars will be able to obtain water from a wide variety of locations. The 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 just be sent out to gather water for colonists.</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>This discovery is significant because it shows the presence of subsurface ice at latitudes further south than expected and proves that future colonists on Mars will be able to obtain water from a wide variety of locations. The 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 just be sent out to gather water for colonists.</div></td></tr>
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<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;">File:ESP 025840 2240-3icecrater.gif|Ice disappering after being exposed by impact.</ins></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>==Dark slope streaks==</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>==Dark slope streaks==</div></td></tr>
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</table>Suitupshowuphttp://marspedia.org/index.php?title=Ismenius_Lacus_quadrangle&diff=140915&oldid=140854Ismenius Lacus quadrangle2024-03-27T17:35:16Z<p><span dir="auto"><span class="autocomment">Dipping layers</span></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>==Dipping layers==</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>==Dipping layers==</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>Scattered around Mars are features that have been called "dipping layers" They are groups of layers in protected place like inside of craters or against slopes. They once covered a wide area, but erosion has since removed most of the material. The material that formed them may fell from the sky as ice-rich dust.<ref>Carr, M. 2001. Mars Global Surveyor observations of martian fretted terrain. J. Geophys. Res. 106, 23571-23593.</ref> <ref>Baker, D., J. Head. 2015. Extensive Middle Amazonian mantling of debris aprons and plains in Deuteronilus Mensae, Mars: Implication for the record of mid-latitude glaciation. Icarus: 260, 269-288</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>Scattered around Mars are features that have been called "dipping layers" They are groups of layers in protected place like inside of craters or against slopes. They once covered a wide area, but erosion has since removed most of the material. The material that formed them may fell from the sky as ice-rich dust.<ref>Carr, M. 2001. Mars Global Surveyor observations of martian fretted terrain. J. Geophys. Res. 106, 23571-23593.</ref> <ref>Baker, D., J. Head. 2015. Extensive Middle Amazonian mantling of debris aprons and plains in Deuteronilus Mensae, Mars: Implication for the record of mid-latitude glaciation. Icarus: 260, 269-288</ref> <ins class="diffchange diffchange-inline"> Another idea for their origin was presented at 55th LPSC (2024) by an international team of researchers. They suggest that the layers are from past ice sheets.<ref>Blanc, E., et al. 2024. ORIGIN OF WIDESPREAD LAYERED DEPOSITS ASSOCIATED WITH MARTIAN DEBRIS COVERED GLACIERS. 55th LPSC (2024). 1466.pdf</ref> </ins></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><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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