Periodic climate changes on Mars - Revision history

Suitupshowup: /* Latitude Dependent Mantle */ added ref

2025-03-13T19:45:18Z

Latitude Dependent Mantle: added ref

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	==Latitude Dependent Mantle==		==Latitude Dependent Mantle==

	Using the ever increasing resolution of cameras orbiting Mars, we have discovered that many parts of the planet are covered by a smooth coating that in some cases is layered and quite thick. This mantle covers at least 23% of the surface.<ref> M.A. Kreslavsky, J.W. Head. Mars: Nature and evolution of young latitude-dependent water–ice-rich mantle: MARS. Geophys. Res. Lett., 29 (2002). </ref> <ref>Jawin, E.,et al. 2018. Transient post-glacial processes on Mars: Geomorphologic evidence for a paraglacial period. Icarus. Volume 309. Pages 187-206</ref> <ref>Mustard, J., C. Cooper, M. Rifkin. 2001. Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice. Nature 412, 411–414 .</ref> Some parts are eroded, revealing rough surfaces. Some parts possess layers. It’s generally accepted that mantle is ice-rich dust that fell from the sky as snow and ice-coated dust grains during a different climate.<ref>Pollack, J., D. Colburn, F. Flaser, R. Kahn, C. Carson, and D. Pidek. 1979. Properties and effects of dust suspended in the martian atmosphere. J. Geophys. Res. 84, 2929-2945. </ref> Latitude Dependent Mantle and many other supposed ice-rich features occur in two rather wide latitude bands in the mid-latitudes: 30-60 degrees North and 30-60 degrees South latitudes.		Using the ever increasing resolution of cameras orbiting Mars, we have discovered that many parts of the planet are covered by a smooth coating that in some cases is layered and quite thick.<ref>Head, J., et al. 2003, Recent ice ages on Mars. Nature. 426.797-802</ref> This mantle covers at least 23% of the surface.<ref> M.A. Kreslavsky, J.W. Head. Mars: Nature and evolution of young latitude-dependent water–ice-rich mantle: MARS. Geophys. Res. Lett., 29 (2002). </ref> <ref>Jawin, E.,et al. 2018. Transient post-glacial processes on Mars: Geomorphologic evidence for a paraglacial period. Icarus. Volume 309. Pages 187-206</ref> <ref>Mustard, J., C. Cooper, M. Rifkin. 2001. Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice. Nature 412, 411–414 .</ref> Some parts are eroded, revealing rough surfaces. Some parts possess layers. It’s generally accepted that mantle is ice-rich dust that fell from the sky as snow and ice-coated dust grains during a different climate.<ref>Pollack, J., D. Colburn, F. Flaser, R. Kahn, C. Carson, and D. Pidek. 1979. Properties and effects of dust suspended in the martian atmosphere. J. Geophys. Res. 84, 2929-2945. </ref> Latitude Dependent Mantle and many other supposed ice-rich features occur in two rather wide latitude bands in the mid-latitudes: 30-60 degrees North and 30-60 degrees South latitudes.
	There are many features with layers that may have been deposited as latitude dependent mantle in past times. Later they were sculptured by winds into strange, beautiful shapes. Some are in craters; others are leaning against steep walls.		There are many features with layers that may have been deposited as latitude dependent mantle in past times. Later they were sculptured by winds into strange, beautiful shapes. Some are in craters; others are leaning against steep walls.
	<gallery class="center" widths="190px" heights="180px">		<gallery class="center" widths="190px" heights="180px">

Suitupshowup: /* Latitude Dependent Mantle */

2023-12-30T01:20:44Z

Latitude Dependent Mantle

← Older revision		Revision as of 02:20, 30 December 2023
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	==Latitude Dependent Mantle==		==Latitude Dependent Mantle==

	Using the ever increasing resolution of cameras orbiting Mars, we have discovered that many parts of the planet are covered by a smooth coating that in some cases is layered and quite thick. This mantle covers at least 23% of the surface.<ref> M.A. Kreslavsky, J.W. Head. Mars: Nature and evolution of young latitude-dependent water–ice-rich mantle: MARS. Geophys. Res. Lett., 29 (2002). ~~14-1–14-4~~		Using the ever increasing resolution of cameras orbiting Mars, we have discovered that many parts of the planet are covered by a smooth coating that in some cases is layered and quite thick. This mantle covers at least 23% of the surface.<ref> M.A. Kreslavsky, J.W. Head. Mars: Nature and evolution of young latitude-dependent water–ice-rich mantle: MARS. Geophys. Res. Lett., 29 (2002). </ref> <ref>Jawin, E.,et al. 2018. Transient post-glacial processes on Mars: Geomorphologic evidence for a paraglacial period. Icarus. Volume 309. Pages 187-206</ref> <ref>Mustard, J., C. Cooper, M. Rifkin. 2001. Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice. Nature 412, 411–414 .</ref> Some parts are eroded, revealing rough surfaces. Some parts possess layers. It’s generally accepted that mantle is ice-rich dust that fell from the sky as snow and ice-coated dust grains during a different climate.<ref>Pollack, J., D. Colburn, F. Flaser, R. Kahn, C. Carson, and D. Pidek. 1979. Properties and effects of dust suspended in the martian atmosphere. J. Geophys. Res. 84, 2929-2945. </ref> Latitude Dependent Mantle and many other supposed ice-rich features occur in two rather wide latitude bands in the mid-latitudes: 30-60 degrees North and 30-60 degrees South latitudes.
	~~https://doi-org.wikipedialibrary.idm.oclc.org/10.1029/2002GL015392~~</ref> <ref>Jawin, E.,et al. 2018. Transient post-glacial processes on Mars: Geomorphologic evidence for a paraglacial period. Icarus. Volume 309. Pages 187-206<ref> <ref>Mustard, J., C. Cooper, M. Rifkin. 2001. Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice. Nature 412, 411–414 .</ref> Some parts are eroded, revealing rough surfaces. Some parts possess layers. It’s generally accepted that mantle is ice-rich dust that fell from the sky as snow and ice-coated dust grains during a different climate.<ref>Pollack, J., D. Colburn, F. Flaser, R. Kahn, C. Carson, and D. Pidek. 1979. Properties and effects of dust suspended in the martian atmosphere. J. Geophys. Res. 84, 2929-2945. </ref> Latitude Dependent Mantle and many other supposed ice-rich features occur in two rather wide latitude bands in the mid-latitudes: 30-60 degrees North and 30-60 degrees South latitudes.
	There are many features with layers that may have been deposited as latitude dependent mantle in past times. Later they were sculptured by winds into strange, beautiful shapes. Some are in craters; others are leaning against steep walls.		There are many features with layers that may have been deposited as latitude dependent mantle in past times. Later they were sculptured by winds into strange, beautiful shapes. Some are in craters; others are leaning against steep walls.
	<gallery class="center" widths="190px" heights="180px">		<gallery class="center" widths="190px" heights="180px">

Suitupshowup: /* Latitude Dependent Mantle */ added ref and new info

2023-12-30T01:19:13Z

Latitude Dependent Mantle: added ref and new info

← Older revision		Revision as of 02:19, 30 December 2023
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	==Latitude Dependent Mantle==		==Latitude Dependent Mantle==

	Using the ever increasing resolution of cameras orbiting Mars, we have discovered that many parts of the planet are covered by a smooth coating that in some cases is layered and quite thick. <ref>Mustard, J., C. Cooper, M. Rifkin. 2001. Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice. Nature 412, 411–414 .</ref> Some parts are eroded, revealing rough surfaces. Some parts possess layers. It’s generally accepted that mantle is ice-rich dust that fell from the sky as snow and ice-coated dust grains during a different climate.<ref>Pollack, J., D. Colburn, F. Flaser, R. Kahn, C. Carson, and D. Pidek. 1979. Properties and effects of dust suspended in the martian atmosphere. J. Geophys. Res. 84, 2929-2945. </ref> Latitude Dependent Mantle and many other supposed ice-rich features occur in two rather wide latitude bands in the mid-latitudes: 30-60 degrees North and 30-60 degrees South latitudes.		Using the ever increasing resolution of cameras orbiting Mars, we have discovered that many parts of the planet are covered by a smooth coating that in some cases is layered and quite thick. This mantle covers at least 23% of the surface.<ref> M.A. Kreslavsky, J.W. Head. Mars: Nature and evolution of young latitude-dependent water–ice-rich mantle: MARS. Geophys. Res. Lett., 29 (2002). 14-1–14-4
			https://doi-org.wikipedialibrary.idm.oclc.org/10.1029/2002GL015392</ref> <ref>Jawin, E.,et al. 2018. Transient post-glacial processes on Mars: Geomorphologic evidence for a paraglacial period. Icarus. Volume 309. Pages 187-206<ref> <ref>Mustard, J., C. Cooper, M. Rifkin. 2001. Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice. Nature 412, 411–414 .</ref> Some parts are eroded, revealing rough surfaces. Some parts possess layers. It’s generally accepted that mantle is ice-rich dust that fell from the sky as snow and ice-coated dust grains during a different climate.<ref>Pollack, J., D. Colburn, F. Flaser, R. Kahn, C. Carson, and D. Pidek. 1979. Properties and effects of dust suspended in the martian atmosphere. J. Geophys. Res. 84, 2929-2945. </ref> Latitude Dependent Mantle and many other supposed ice-rich features occur in two rather wide latitude bands in the mid-latitudes: 30-60 degrees North and 30-60 degrees South latitudes.
	There are many features with layers that may have been deposited as latitude dependent mantle in past times. Later they were sculptured by winds into strange, beautiful shapes. Some are in craters; others are leaning against steep walls.		There are many features with layers that may have been deposited as latitude dependent mantle in past times. Later they were sculptured by winds into strange, beautiful shapes. Some are in craters; others are leaning against steep walls.
	<gallery class="center" widths="190px" heights="180px">		<gallery class="center" widths="190px" heights="180px">

Suitupshowup: /* External links */ added link

2023-12-30T01:13:20Z

External links: added link

← Older revision		Revision as of 02:13, 30 December 2023
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	*[https://www.youtube.com/watch?v=_sUUKcZaTgA Martian Ice - Jim Secosky - 16th Annual International Mars Society Convention]		*[https://www.youtube.com/watch?v=_sUUKcZaTgA Martian Ice - Jim Secosky - 16th Annual International Mars Society Convention]

			*Jawin, E.,et al. 2018. Transient post-glacial processes on Mars: Geomorphologic evidence for a paraglacial period. Icarus. Volume 309. Pages 187-206


	[[category:climate]]		[[category:climate]]

RichardWSmith: Pointed out that periods of high axial tilt result in a generally warmer, wetter planet.

2021-03-03T07:23:31Z

Pointed out that periods of high axial tilt result in a generally warmer, wetter planet.

Show changes

Suitupandshowup: added ref

2020-12-26T16:19:43Z

added ref

← Older revision		Revision as of 17:19, 26 December 2020
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	Article written by Jim Secosky. Jim is a retired science teacher who has used the Hubble Space Telescope, the Mars Global Surveyor, and HiRISE.		Article written by Jim Secosky. Jim is a retired science teacher who has used the Hubble Space Telescope, the Mars Global Surveyor, and HiRISE.

	Many features on Mars contain large amounts of ice. Many of these have formed beautiful forms. The most popular model for the origin of the ice is climate changes caused by large changes in the tilt of the planet's rotational axis. At times the tilt has even been greater than 80 degrees.		Many features on Mars contain large amounts of ice. Many of these have formed beautiful forms. The most popular model for the origin of the ice is climate changes caused by large changes in the tilt of the planet's rotational axis.<ref>https://www.uahirise.org/hipod/ESP_034132_1750</ref> At times the tilt has even been greater than 80 degrees.
	<ref> last1 = Touma \| first1 = J. \| last2 = Wisdom \| first2 = J. \| year = 1993 \| title = The Chaotic Obliquity of Mars \| url = \| journal = Science \| volume = 259 \| issue = \| pages = 1294–1297 \| doi=10.1126/science.259.5099.1294\| </ref> <ref > \| last1 = Laskar \| first1 = J. \| last2 = Correia \| first2 = A. \| last3 = Gastineau \| first3 = M. \| last4 = Joutel \| first4 = F. \| last5 = Levrard \| first5 = B. \| last6 = Robutel \| first6 = P. \| year = 2004 \| title = Long term evolution and chaotic diffusion of the insolation quantities of Mars \| url = \| journal = Icarus \| volume = 170 \| issue = \| pages = 343–364 \| doi=10.1016/j.icarus.2004.04.005 \| </ref>		<ref> last1 = Touma \| first1 = J. \| last2 = Wisdom \| first2 = J. \| year = 1993 \| title = The Chaotic Obliquity of Mars \| url = \| journal = Science \| volume = 259 \| issue = \| pages = 1294–1297 \| doi=10.1126/science.259.5099.1294\| </ref> <ref > \| last1 = Laskar \| first1 = J. \| last2 = Correia \| first2 = A. \| last3 = Gastineau \| first3 = M. \| last4 = Joutel \| first4 = F. \| last5 = Levrard \| first5 = B. \| last6 = Robutel \| first6 = P. \| year = 2004 \| title = Long term evolution and chaotic diffusion of the insolation quantities of Mars \| url = \| journal = Icarus \| volume = 170 \| issue = \| pages = 343–364 \| doi=10.1016/j.icarus.2004.04.005 \| </ref>
	Large changes in the tilt explains how some places on Mars accumulated ice. Studies have shown that when the tilt of Mars reaches 45 degrees from its current 25 degrees, ice is no longer stable at the poles.		Large changes in the tilt explains how some places on Mars accumulated ice. Studies have shown that when the tilt of Mars reaches 45 degrees from its current 25 degrees, ice is no longer stable at the poles.

Suitupandshowup at 22:33, 21 March 2020

2020-03-21T22:33:46Z

← Older revision		Revision as of 23:33, 21 March 2020
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	</gallery>		</gallery>

	<gallery class="center" widths="~~190px~~" heights="~~180px~~">
			<gallery class="center" widths="380px" heights="360px">

	File:ESP 054934 2160pyramid.jpg\|Mantle layers eroded and shaped by winds		File:ESP 054934 2160pyramid.jpg\|Mantle layers eroded and shaped by winds
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	Some bare an uncanny resemblance to alpine or mountain glaciers of the Earth. These, supposed alpine glaciers, have been called glacier-like forms (GLF) or glacier-like flows (GLF). <ref> Arfstrom, J and W. Hartmann. 2005. Martian flow features, moraine-like ridges, and gullies: Terrestrial analogs and interrelationships. Icarus 174, 321-335.</ref> <ref> Hubbard B., R. Milliken, J. Kargel , A. Limaye, C. Souness . 2011. Geomorphological characterization and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars Icarus 211, 330–346 </ref> Another, more general term sometimes seen in the literature is viscous flow features (VFF). <ref> Hubbard B., R. Milliken, J. Kargel , A. Limaye, C. Souness . 2011. Geomorphological characterization and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars Icarus 211, 330–346 </ref>		Some bare an uncanny resemblance to alpine or mountain glaciers of the Earth. These, supposed alpine glaciers, have been called glacier-like forms (GLF) or glacier-like flows (GLF). <ref> Arfstrom, J and W. Hartmann. 2005. Martian flow features, moraine-like ridges, and gullies: Terrestrial analogs and interrelationships. Icarus 174, 321-335.</ref> <ref> Hubbard B., R. Milliken, J. Kargel , A. Limaye, C. Souness . 2011. Geomorphological characterization and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars Icarus 211, 330–346 </ref> Another, more general term sometimes seen in the literature is viscous flow features (VFF). <ref> Hubbard B., R. Milliken, J. Kargel , A. Limaye, C. Souness . 2011. Geomorphological characterization and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars Icarus 211, 330–346 </ref>

	<gallery class="center" widths="~~190px~~" heights="~~180px~~" >
			<gallery class="center" widths="380px" heights="360px">

	File:ESP 018857 2225alpineglacier.jpg \|Alpine glacier moving from a valley Lat: 42.2° N Long: 50.5° E (309.5 W)		File:ESP 018857 2225alpineglacier.jpg \|Alpine glacier moving from a valley Lat: 42.2° N Long: 50.5° E (309.5 W)
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	==Ice Cap Layers==		==Ice Cap Layers==

	A sign that the Martian climate has changed was discovered early on in the northern ice cap of Mars. It displays many layers of ice that accumulated when the climate changed. These are visible in the walls of canyons.		A sign that the Martian climate has changed was discovered early on in the northern ice cap of Mars. It displays many layers of ice that accumulated when the climate changed. These are visible in the walls of canyons.
	<gallery class="center" widths="~~190px~~" heights="~~180px~~" >

			<gallery class="center" widths="380px" heights="360px">
	File:ESP 044934 2670icecaplayers.jpg\|Layers exposed in ice cap in Mare Boreum quadrangle		File:ESP 044934 2670icecaplayers.jpg\|Layers exposed in ice cap in Mare Boreum quadrangle
	File:ESP 036863 2670icecaplayers.jpg\| Layers exposed in ice cap in Mare Boreum quadrangle		File:ESP 036863 2670icecaplayers.jpg\| Layers exposed in ice cap in Mare Boreum quadrangle
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	Brain terrain is a region of maze-like ridges 3–5 meters high. Brain terrain probably stars when cracks form in ice-rich ground—ground that was produced when the climate was different. Along the cracks there is increased [[sublimation]] of ice. As more and more ice disappears by sublimation, the cracks widen. Some ridges may consist of an ice core, so they may be sources of water for future colonists.<ref> Levy, J., J. Head, D. Marchant. 2009. Concentric crater fill in Utopia Planitia: History and interaction between glacial “brain terrain” and periglacial mantle processes. Icarus 202, 462–476.</ref>		Brain terrain is a region of maze-like ridges 3–5 meters high. Brain terrain probably stars when cracks form in ice-rich ground—ground that was produced when the climate was different. Along the cracks there is increased [[sublimation]] of ice. As more and more ice disappears by sublimation, the cracks widen. Some ridges may consist of an ice core, so they may be sources of water for future colonists.<ref> Levy, J., J. Head, D. Marchant. 2009. Concentric crater fill in Utopia Planitia: History and interaction between glacial “brain terrain” and periglacial mantle processes. Icarus 202, 462–476.</ref>
	<gallery class="center" widths="~~190px~~" heights="~~180px~~" >

			<gallery class="center" widths="380px" heights="360px">
	File:54526 2220brainscracks.jpg\|Brain terrain and a field of cracks that will develop into brain terrain, as sublimation takes place along the crack surfaces		File:54526 2220brainscracks.jpg\|Brain terrain and a field of cracks that will develop into brain terrain, as sublimation takes place along the crack surfaces
	File:54996 2155brains.jpg\|Close, color view of brain terrain		File:54996 2155brains.jpg\|Close, color view of brain terrain
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	[[sublimation]]." So much of the ground is ice that when the ice disappears the ground collapses. The ice goes into the atmosphere. Dust left behind is eventually just blown away, leaving wide valleys and hollows.<ref>https://en.wikipedia.org/wiki/Upper_Plains_Unit</ref>		[[sublimation]]." So much of the ground is ice that when the ice disappears the ground collapses. The ice goes into the atmosphere. Dust left behind is eventually just blown away, leaving wide valleys and hollows.<ref>https://en.wikipedia.org/wiki/Upper_Plains_Unit</ref>

	<gallery class="center" widths="~~190px~~" heights="~~180px~~" >
			<gallery class="center" widths="380px" heights="360px">
	File:ESP 047499 2245ribswide.jpg\|Wide view of ribbed terrain in Ismenius Lacus quadrangle		File:ESP 047499 2245ribswide.jpg\|Wide view of ribbed terrain in Ismenius Lacus quadrangle
	File:ESP 028339 2245headarticle.jpg\|Ribbed terrain in Ismenius Lacus quadrangle		File:ESP 028339 2245headarticle.jpg\|Ribbed terrain in Ismenius Lacus quadrangle

Suitupandshowup: /* Ribbed Terrain */

2019-02-08T15:56:43Z

Ribbed Terrain

← Older revision		Revision as of 16:56, 8 February 2019
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	File:54896 2240hollow.jpg\|Hollowed terrain Some of the cracks visible in image may eventually turn into ribbed or hollowed terrain, as sublimation progresses		File:54896 2240hollow.jpg\|Hollowed terrain Some of the cracks visible in image may eventually turn into ribbed or hollowed terrain, as sublimation progresses
	~~File:ESP 054896 2240hollowsrelease.jpg\|Close, color view of hollowed terrain~~
	</gallery>		</gallery>

	[[File:ESP 054896 2240hollowsrelease.jpg\|center\|thumb\|400px\|Close, color view of hollowed terrain]]		[[File:ESP 054896 2240hollowsrelease.jpg\|center\|thumb\|400px\|Close, color view of hollowed terrain]]


	==References==		==References==

Suitupandshowup at 15:56, 8 February 2019

2019-02-08T15:56:13Z

← Older revision		Revision as of 16:56, 8 February 2019
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	File:ESP 035208 2215brainslabeledmarspedia.jpg\|Wide view of brain terrain in the Ismenius Lacus quadrangle		File:ESP 035208 2215brainslabeledmarspedia.jpg\|Wide view of brain terrain in the Ismenius Lacus quadrangle
	~~File:45917 2220brainsforming.jpg\|Brain terrain forming in Ismenius Lacus quadrangle~~
	</gallery>		</gallery>

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	[[File:45917 2220brainsforming.jpg\|center\|thumb\|400px\|Brain terrain forming in Ismenius Lacus quadrangle]]		[[File:45917 2220brainsforming.jpg\|center\|thumb\|400px\|Brain terrain forming in Ismenius Lacus quadrangle]]

	==Ribbed ~~terrain~~==		==Ribbed Terrain==

	Ribbed terrain forms as ice leaves the ground along cracks in a process called "		Ribbed terrain forms as ice leaves the ground along cracks in a process called "
	[[sublimation]]." So much of the ground is ice that when the ice disappears the ground collapses. The ice goes into the atmosphere. Dust left behind is eventually just blown away, leaving wide valleys and hollows.<ref>https://en.wikipedia.org/wiki/Upper_Plains_Unit</ref>		[[sublimation]]." So much of the ground is ice that when the ice disappears the ground collapses. The ice goes into the atmosphere. Dust left behind is eventually just blown away, leaving wide valleys and hollows.<ref>https://en.wikipedia.org/wiki/Upper_Plains_Unit</ref>
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	File:ESP 054896 2240hollowsrelease.jpg\|Close, color view of hollowed terrain		File:ESP 054896 2240hollowsrelease.jpg\|Close, color view of hollowed terrain
	</gallery>		</gallery>

			[[File:ESP 054896 2240hollowsrelease.jpg\|center\|thumb\|400px\|Close, color view of hollowed terrain]]


	==References==		==References==
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	==See Also==		==See Also==

	*[[Glaciers on Mars]]		*[[Glaciers on Mars]]
	*[[High Resolution Imaging Science Experiment (HiRISE)]]		*[[High Resolution Imaging Science Experiment (HiRISE)]]

Suitupandshowup: /* Brain Terrain */

2019-02-08T15:53:57Z

Brain Terrain

← Older revision		Revision as of 16:53, 8 February 2019
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	File:45917 2220brainsforming.jpg\|Brain terrain forming in Ismenius Lacus quadrangle		File:45917 2220brainsforming.jpg\|Brain terrain forming in Ismenius Lacus quadrangle
	</gallery>		</gallery>


			[[File:45917 2220brainsforming.jpg\|center\|thumb\|400px\|Brain terrain forming in Ismenius Lacus quadrangle]]

	==Ribbed terrain==		==Ribbed terrain==