HiRISE observations of gas sublimation-driven activity in Mars’ southern polar regions: II. Surficial deposits and their origins

Thomas, N.; Hansen, C. J.; Portyankina, Ganna; Russell, P. S.

doi:10.1016/j.icarus.2009.05.030

Cited by 57 publications

(56 citation statements)

References 22 publications

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“…This study was inspired by the set of papers discussing sublimation phenomena in the southern seasonal polar cap and their connection to the solid state greenhouse effect (Pommerol et al, 2011a;Hansen et al, 2010;Thomas et al, 2010;Portyankina et al, 2010). With an aim to evaluate the level of similarity of phenomena observed in both hemispheres we provided a description of spring seasonal activity in four places inside the north polar erg: Arrakis, Buzzel, Kolhar, and Kaitain.…”

Section: Discussionmentioning

confidence: 99%

Observations of the northern seasonal polar cap on Mars II: HiRISE photometric analysis of evolution of northern polar dunes in spring

Portyankina

Pommerol

Aye

et al. 2013

Icarus

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Section: Discussionmentioning

confidence: 99%

Observations of the northern seasonal polar cap on Mars II: HiRISE photometric analysis of evolution of northern polar dunes in spring

Portyankina

Pommerol

Aye

et al. 2013

Icarus

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“…They range in size from tens of meters up to about one kilometer, with typical diameters of 200–300 m. Channel depths of 0.6 to 1 m have been estimated for typical 5 m wide channels [ Hansen et al , 2010; Piqueux et al , 2003]. During the Martian spring, these unusual patterns are associated with the transient formation of dark fan‐shaped dust deposits, which are formed in approximately the same positions each year, indicating that local topographic features are important for their formation [ Thomas et al , 2010]. [ Piqueux and Christensen , 2008] suggested a minimum formation time on the order of 10 4 years, based on estimates of the volume of granular material that must be excavated to form the central depression and the amount of granular material in a typical fan‐shaped deposit.…”

Section: Introductionmentioning

confidence: 99%

Formation of Martian araneiforms by gas‐driven erosion of granular material

Villiers

Nermoen

Jamtveit

et al. 2012

Geophysical Research Letters

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Sublimation at the lower surface of a seasonal sheet of translucent CO2 ice at high southern latitudes during the Martian spring, and rapid outflow of the CO2 gas generated in this manner through holes in the ice, has been proposed as the origin of dendritic 100 m–1 km scale branched channels known as spiders or araneiforms and dark dust fans deposited on top of the ice. We show that patterns very similar to araneiforms are formed in a Hele‐Shaw cell filled with an unconsolidated granular material by slowly deforming the upper wall upward and allowing it to return rapidly to its original position to drive air and entrained particles through a small hole in the upper wall. Straight, braided and quasiperiodic oscillating channels, unlike meandering channels on Earth were also formed.

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“…Pilorget et al [] have modeled this process and demonstrated that basal sublimation is indeed expected to occur on Mars in the case of a clean large‐grained CO 2 ice (grain size typically greater than a few centimeter and dust content less than a few tens of parts per million). Other surveys using HiRISE and CRISM observations have also supported this explanation [ Titus et al , ; Hansen et al , ; Thomas et al , ; Pommerol et al , ]. This process is proposed to be a major erosive agent in the polar regions and thus could significantly affect the preservation of the near‐surface stratigraphic record [ Piqueux and Christensen , ; Hansen et al , ].…”

Section: Introductionmentioning

confidence: 88%

Material ejection by the cold jets and temperature evolution of the south seasonal polar cap of Mars from THEMIS/CRISM observations and implications for surface properties

et al. 2013

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[1] As the seasonal CO 2 ice polar caps of Mars retreat during spring, dark spots appear on the ice in some specific regions. These features are thought to result from basal sublimation of the transparent CO 2 ice followed by ejection of regolith-type material, which then covers the ice. We have used Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) reflectance data, Thermal Emission Imaging System (THEMIS) visible images, and THEMIS-derived temperature retrievals along with a thermal numerical model to constrain the physical and compositional characteristics of the seasonal cap for several areas exhibiting dark spots at both high spatial and temporal resolutions. Data analysis suggests an active period of material ejection (before solar longitude (Ls) 200), accumulation around the ejection points, and spreading of part of the ejected material over the whole area, followed by a period where no significant amount of material is ejected, followed by complete defrosting ( Ls 245). Dark material thickness on top of the CO 2 ice is estimated to range from a few hundreds of microns to a few millimeters in the warmest spots, based on numerical modeling combined with the observed temperature evolution. The nature of the venting process and the amount of material that is moved lead to the conclusion that it could have an important impact on the surface physical properties.Citation: Pilorget, C., C. S. Edwards, B. L. Ehlmann, F. Forget, and E. Millour (2013), Material ejection by the cold jets and temperature evolution of the south seasonal polar cap of Mars from THEMIS/CRISM observations and implications for surface properties,

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HiRISE observations of gas sublimation-driven activity in Mars’ southern polar regions: II. Surficial deposits and their origins

Cited by 57 publications

References 22 publications

Observations of the northern seasonal polar cap on Mars II: HiRISE photometric analysis of evolution of northern polar dunes in spring

Observations of the northern seasonal polar cap on Mars II: HiRISE photometric analysis of evolution of northern polar dunes in spring

Formation of Martian araneiforms by gas‐driven erosion of granular material

Material ejection by the cold jets and temperature evolution of the south seasonal polar cap of Mars from THEMIS/CRISM observations and implications for surface properties

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