Carbonates on Mars
Head (vessel) Evidence for carbonates on Mars was first discovered in 2008. Previously, most remote sensing instruments such as OMEGA and THEMIS —sensitive to infrared emissivity spectral features of carbonates —had not suggested the presence of carbonate outcrops, [1] at least at the 100 m or coarser spatial scales available from the returned data. [2]
Page Revisions
| Year | Metadata | Sections | Top Words | First Paragraph |
| 2018 |
66173 characters 4 sections 9 paragraphs 8 images 190 internal links 42 external links |
carbonate 0.505 carbonates 0.422 ph 0.194 minerals 0.166 magnesite 0.135 gusev 0.118 outcrops 0.116 aqueous 0.111 alteration 0.109 deposit 0.105 huygens 0.100 nili 0.093 spectral 0.086 crism 0.078 outcrop 0.077 |
Head (vessel) Evidence for carbonates on Mars was first discovered in 2008. Previously, most remote sensing instruments such as OMEGA and THEMIS —sensitive to infrared emissivity spectral features of carbonates —had not suggested the presence of carbonate outcrops, [1] at least at the 100 m or coarser spatial scales available from the returned data. [2] |
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| 2017 |
63599 characters 4 sections 9 paragraphs 8 images 190 internal links 36 external links |
carbonate 0.505 carbonates 0.422 ph 0.194 minerals 0.166 magnesite 0.135 gusev 0.118 outcrops 0.116 aqueous 0.111 alteration 0.109 deposit 0.105 huygens 0.100 nili 0.093 spectral 0.086 crism 0.078 outcrop 0.077 |
Head (vessel) Evidence for carbonates on Mars was first discovered in 2008. Previously, most remote sensing instruments such as OMEGA and THEMIS —sensitive to infrared emissivity spectral features of carbonates —had not suggested the presence of carbonate outcrops, [1] at least at the 100 m or coarser spatial scales available from the returned data. [2] |
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| 2016 |
63596 characters 4 sections 9 paragraphs 8 images 190 internal links 36 external links |
carbonate 0.505 carbonates 0.422 ph 0.194 minerals 0.166 magnesite 0.135 gusev 0.118 outcrops 0.116 aqueous 0.111 alteration 0.109 deposit 0.105 huygens 0.100 nili 0.093 spectral 0.086 crism 0.078 outcrop 0.077 |
Head (vessel) Evidence for carbonates on Mars was first discovered in 2008. Previously, most remote sensing instruments such as OMEGA and THEMIS —sensitive to infrared emissivity spectral features of carbonates —had not suggested the presence of carbonate outcrops, [1] at least at the 100 m or coarser spatial scales available from the returned data. [2] |
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| 2015 |
60251 characters 3 sections 8 paragraphs 7 images 180 internal links 36 external links |
carbonate 0.506 carbonates 0.423 ph 0.194 minerals 0.167 magnesite 0.136 gusev 0.119 outcrops 0.116 aqueous 0.111 alteration 0.109 deposit 0.106 huygens 0.101 nili 0.093 spectral 0.087 crism 0.078 outcrop 0.078 |
Evidence for carbonates on Mars has remained elusive until recently. For example, most remote sensing instruments such as OMEGA and THEMIS that are sensitive to infrared emissivity spectral features of carbonates , had not suggested the presence of carbonate outcrops [1] at 100 m or coarser spatial scales. [2] Though ubiquitous, carbonates dominated by Magnesite (MgCO 3 ) in Martian dust had mass fractions less than 5% and could have formed under current atmospheric conditions. [3] Furthermore, with the exception of the surface dust component, carbonates had not been detected by any in situ mission, even though mineralogic modeling does not preclude small amounts of calcium carbonate in Independence class rocks of Husband Hill in Gusev crater [4] (note: An IAU naming convention within Gusev is not yet established). |
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| 2014 |
60067 characters 2 sections 7 paragraphs 5 images 180 internal links 36 external links |
carbonate 0.483 carbonates 0.433 ph 0.199 minerals 0.171 magnesite 0.139 gusev 0.121 outcrops 0.119 aqueous 0.113 alteration 0.112 huygens 0.103 spectral 0.089 deposit 0.081 crism 0.080 outcrop 0.079 feco3 0.077 |
Evidence for carbonates on Mars has remained elusive until recently. For example, most remote sensing instruments such as OMEGA and THEMIS that are sensitive to infrared emissivity spectral features of carbonates , had not suggested the presence of carbonate outcrops [1] at 100 m or coarser spatial scales. [2] Though ubiquitous, carbonates dominated by Magnesite (MgCO 3 ) in Martian dust had mass fractions less than 5% and could have formed under current atmospheric conditions. [3] Furthermore, with the exception of the surface dust component, carbonates had not been detected by any in situ mission, even though mineralogic modeling does not preclude small amounts of calcium carbonate in Independence class rocks of Husband Hill in Gusev crater [4] (note: An IAU naming convention within Gusev is not yet established). |
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| 2013 |
57646 characters 2 sections 7 paragraphs 5 images 179 internal links 35 external links |
carbonate 0.483 carbonates 0.433 ph 0.199 minerals 0.171 magnesite 0.139 gusev 0.121 outcrops 0.119 aqueous 0.113 alteration 0.112 huygens 0.103 spectral 0.089 deposit 0.081 crism 0.080 outcrop 0.079 feco3 0.077 |
Evidence for carbonates on Mars has remained elusive until recently. For example, most remote sensing instruments such as OMEGA and THEMIS that are sensitive to infrared emissivity spectral features of carbonates , had not suggested the presence of carbonate outcrops [1] at 100 m or coarser spatial scales. [2] Though ubiquitous, carbonates dominated by Magnesite (MgCO 3 ) in Martian dust had mass fractions less than 5% and could have formed under current atmospheric conditions. [3] Furthermore, with the exception of the surface dust component, carbonates had not been detected by any in situ mission, even though mineralogic modeling does not preclude small amounts of calcium carbonate in Independence class rocks of Husband Hill in Gusev crater [4] (note: An IAU naming convention within Gusev is not yet established). |
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| 2012 |
56521 characters 2 sections 7 paragraphs 4 images 180 internal links 35 external links |
carbonate 0.483 carbonates 0.433 ph 0.199 minerals 0.171 magnesite 0.139 gusev 0.121 outcrops 0.119 aqueous 0.113 alteration 0.112 huygens 0.103 spectral 0.089 deposit 0.081 crism 0.080 outcrop 0.079 feco3 0.077 |
Evidence for carbonates on Mars has remained elusive until recently. For example, most remote sensing instruments such as OMEGA and THEMIS that are sensitive to infrared emissivity spectral features of carbonates , had not suggested the presence of carbonate outcrops [1] at 100 m or coarser spatial scales. [2] Though ubiquitous, carbonates dominated by Magnesite (MgCO 3 ) in Martian dust had mass fractions less than 5% and could have formed under current atmospheric conditions. [3] Furthermore, with the exception of the surface dust component, carbonates had not been detected by any in situ mission, even though mineralogic modeling does not preclude small amounts of calcium carbonate in Independence class rocks of Husband Hill in Gusev crater [4] (note: An IAU naming convention within Gusev is not yet established). |
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| 2011 |
50217 characters 2 sections 4 paragraphs 3 images 171 internal links 27 external links |
carbonate 0.451 ph 0.260 carbonates 0.257 magnesite 0.181 gusev 0.159 outcrops 0.156 aqueous 0.148 alteration 0.146 spectral 0.116 feco3 0.101 lithic 0.101 mgco3 0.101 mineralogic 0.101 morphology 0.100 modeling 0.099 |
Evidence for carbonates on Mars has remained elusive until recently. For example, most remote sensing instruments such as OMEGA and THEMIS that are sensitive to infrared emissivity spectral features of carbonates , had not suggested the presence of carbonate outcrops [1] at 100 m or coarser spatial scales. [2] Though ubiquitous, carbonates dominated by Magnesite (MgCO 3 ) in Martian dust had mass fractions less than 5% and could have formed under current atmospheric conditions. [3] Furthermore, with the exception of the surface dust component, carbonates had not been detected by any in situ mission, even though mineralogic modeling does not preclude small amounts of calcium carbonate in Independence class rocks of Husband Hill in Gusev crater [4] (note: An IAU naming convention within Gusev is not yet established). |
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| 2010 |
44999 characters 2 sections 4 paragraphs 3 images 170 internal links 12 external links |
carbonate 0.451 ph 0.260 carbonates 0.257 magnesite 0.181 gusev 0.159 outcrops 0.156 aqueous 0.148 alteration 0.146 spectral 0.116 feco3 0.101 lithic 0.101 mgco3 0.101 mineralogic 0.101 morphology 0.100 modeling 0.099 |
Evidence for carbonates on Mars has remained elusive until recently. For example, most remote sensing instruments such as OMEGA and THEMIS that are sensitive to infrared emissivity spectral features of carbonates , had not suggested the presence of carbonate outcrops [1] at 100 m or coarser spatial scales. [2] Though ubiquitous, carbonates dominated by Magnesite (MgCO 3 ) in Martian dust had mass fractions less than 5% and could have formed under current atmospheric conditions. [3] Furthermore, with the exception of the surface dust component, carbonates had not been detected by any in situ mission, even though mineralogic modeling does not preclude small amounts of calcium carbonate in Independence class rocks of Husband Hill in Gusev crater [4] (note: An IAU naming convention within Gusev is not yet established). |
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| 2009 |
61885 characters 2 sections 5 paragraphs 4 images 188 internal links 19 external links |
carbonates 0.311 carbonate 0.307 ph 0.274 alteration 0.184 mineralogic 0.152 aqueous 0.149 magnesite 0.137 olivine 0.131 noachian 0.124 gusev 0.120 outcrops 0.118 fractions 0.113 conditions 0.111 eras 0.110 clays 0.107 |
Evidence for carbonates on Mars has remained elusive. For example, most remote sensing instruments such as OMEGA and THEMIS that are sensitive to infrared emissivity spectral features of carbonates , have not suggested the presence of carbonate outcrops [1] at 100 m or coarser spatial scales. [2] Though ubiquitous, carbonates dominated by Magnesite (MgCO 3 ) in Martian dust have mass fractions less than 5% and can form under current atmospheric conditions. [3] . Furthermore, with the exception of the surface dust component, carbonates have not been detected by any in situ mission, even though mineralogic modeling does not preclude small amounts of calcium carbonate in Independence class rocks of Husband Hill in Gusev crater [4] (note: An IAU naming convention within Gusev is not yet established). |
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| 2008 |
60783 characters 2 sections 5 paragraphs 3 images 189 internal links 19 external links |
carbonates 0.311 carbonate 0.307 ph 0.275 alteration 0.184 mineralogic 0.152 aqueous 0.149 magnesite 0.137 olivine 0.131 noachian 0.125 gusev 0.120 outcrops 0.118 fractions 0.114 conditions 0.112 eras 0.110 clays 0.107 |
Evidence for carbonates on Mars has remained elusive. For example, most remote sensing instruments such as OMEGA and THEMIS that are sensitive to infrared emissivity spectral features of carbonates , have not suggested the presence of carbonate outcrops [1] at 100 m or coarser spatial scales [2] . Though ubiquitous, carbonates dominated by Magnesite (MgCO 3 ) in Martian dust have mass fractions less than 5% and can form under current atmospheric conditions [3] . Furthermore, with the exception of the surface dust component, carbonates have not been detected by any in situ mission, even though mineralogic modeling does not preclude small amounts of calcium carbonate in Independence class rocks of Husband Hill in Gusev crater [4] (note: An IAU naming convention within Gusev is not yet established). |
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| 2007 |
31744 characters 2 sections 5 paragraphs 0 images 40 internal links 16 external links |
carbonates 0.352 carbonate 0.264 ph 0.253 mineralogic 0.196 gusev 0.155 fractions 0.147 clays 0.138 inventory 0.133 magmas 0.133 bulk 0.129 husband 0.128 noachian 0.121 acidic 0.105 outcrops 0.101 feco3 0.098 |
Evidence for carbonates on Mars has remained elusive. For example, in spite of remote sensing instruments such as OMEGA and THEMIS that are sensitive to infrared emissivity spectral features of carbonates , carbonate outcrops have not been detected [1] at 100 m or coarser spatial scales [2] . Though ubiquitous, carbonates dominated by Magnesite (MgCO 3 ) in Martian dust have mass fractions less than 5% and can form under current atmospheric conditions [3] . Furthermore, with the exception of the surface dust component, carbonates have not been detected by any in situ mission, even though mineralogic modeling does not preclude small amounts of calcium carbonate in Independence class rocks of Husband Hill in Gusev crater [4] (note: An IAU naming convention within Gusev is not yet established). |