Amazonian modification of Moreux crater: Record of recent and episodic glaciation in the Protonilus Mensae region of Mars

Sinha, Rishitosh K.; Murty, S. V. S.

doi:10.1016/j.icarus.2014.09.028

Cited by 15 publications

(23 citation statements)

References 92 publications

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“…The CSFD for crater diameters larger than 200 m are well approximated by a 1.5 Ga model isochron, assuming the Hartmann ( 2005) model. This is broadly similar to the crater-count age estimate derived by Sinha and Murty (2015).…”

Section: Appendixsupporting

confidence: 86%

“…Heretofore, much of the discussion about periglaciation on Mars has focused on its relative recentness and the glaciation that preceded it (e.g. Mustard et al, 2001;Head et al, 2003;Levy et al, 2009a, b;Séjourné et al, 2011;Schon et al, 2012;Sinha and Murty, 2015). The older estimation of periglaciation in our study region and the intertwined chronology of two (possible) periglacial periods and three glacial stades documented here suggests that the cycling of the two environment types could be much more Earth-like and extend much more deeply into Mars' history than had been thought hitherto.…”

Section: Discussionmentioning

confidence: 99%

“…Relatively recent work within the Mars community has begun to dissect the mid-to higher-latitudinal terrain of Mars for analogical evidence of similar cold-climate cyclicity and succession (e.g. Dickson et al, 2008;Levy et al, 2009;Baker et al, 2015;Hubbard et al, 2011;Souness and Hubbard, 2013;Sinha and Murty, 2015;Hepburn et al, 2020).…”

Section: Introductionmentioning

confidence: 99%

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Possible polyphase periglaciation and glaciation adjacent to the Moreux impact-crater, Mars

Soare

Conway

Williams

et al. 2021

Icarus

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Section: Appendixsupporting

confidence: 86%

Section: Discussionmentioning

confidence: 99%

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Possible polyphase periglaciation and glaciation adjacent to the Moreux impact-crater, Mars

Soare

Conway

Williams

et al. 2021

Icarus

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“…Although water ice is not presently stable across much of Mars' mid-latitudes (Mellon and Jakosky, 1995;Mellon et al, 2004), evidence of pervasive ice-rich landforms between 30 and 60 o latitude has been presented (Sharp, 1973;Squyres, 1978Squyres, , 1979Lucchitta, 1984;Mangold, 2003;Levy et al, 2007;Baker et al, 2010;Dickson et al, 2010;Head et al, 2010, Souness et al, 2012Hubbard et al, 2014;Brough et al, 2016;Sinha and Murty, 2015). Based on evidence from the Shallow Radar (SHARAD) instrument on board the Mars Reconnaissance Orbiter (MRO), the composition of these ice-rich deposits is consistent with water ice (Holt et al, 2008;Plaut et al, 2009), and their surface morphologies are indicative of viscous flow of that ice (e.g.…”

Section: Introductionmentioning

confidence: 99%

Former extent of glacier-like forms on Mars

Brough

Hubbard

2016

Icarus

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This is the author accepted manuscript. The final version is available from Elsevier via http://dx.doi.org/10.1016/j.icarus.2016.03.006Mars? mid-latitude glacier-like forms (GLFs) have undergone substantial mass loss and recession since a hypothesised last martian glacial maximum (LMGM) stand. To date, there is a lack of knowledge of the nature and timing of the LMGM, the subsequent mass loss and whether this mass loss has been spatially variable. Here, we present the results of a population-scale inventory of recessional GLFs, derived from analysis of 1293 GLFs identified within Context Camera (CTX) imagery, to assess the distribution and controls on GLF recession. A total of 436 GLFs were identified showing strong evidence of recession: 197 in the northern hemisphere and 239 in the southern hemisphere. Relative to their parent populations, recessional GLFs are over-represented in the low latitude belts between 25 and 40o and in areas of high relief, suggesting that these zones exert some control over GLF sensitivity and response to forcing. This analysis is complemented by the reconstruction of the maximum extent and morphology of a specific GLF for which High Resolution Imaging Science Experiment (HiRISE) derived digital elevation data are available. Using Nye?s (Nye, J. F. [1951] Proc. Roy. Soc. Lond, Ser. A-Mat. Phys. Sci, 207, 554-572) perfect plastic approximation of ice flow applied to multiple flow-lines under an optimum yield strength of 22 kPa, we calculate that the reconstructed GLF has lost an area of 6.86 km2 with a corresponding volume loss of 0.31 km3 since the LMGM. Assuming the loss reconstructed at this GLF occurred at all mid-latitude GLFs yields a total planetary ice loss from Mars? GLFs of 135 km3, similar to the current ice volume in the European Alps on Earth.authorsversionPeer reviewe

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“…The suite of Late Amazonian landforms in the middle latitudes (30˚-60˚ N&S hemispheres) has suggested that the last 10 million to 1 billion years of Mars is dominated by multiple episodes of glaciation resulting in flow of ice-rich material [1][2][3][4][5][6][7][8][9][10][11] . A class of ice-rich landforms resulting from flow of ice-rich material during the Late Amazonian glacial episodes includes lobate debris aprons (LDA), linear valley fills (LFF), concentric crater fills (CCF), viscous flow features (VFF) and lobate flow features (LFF).…”

Section: Introductionmentioning

confidence: 99%

Terrestrial rock glaciers: a potential analog for Martian lobate flow features (LFF)

2016

Self Cite

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Rock glaciers, regarded as cryospheric ice/water resource in the terrestrial-glacial systems based on their tongue/lobateshaped flow characteristic and subsurface investigation using ground-penetrating radar. We examined the subsurface, geomorphology, climate-sensitivity and thermophysical properties of a Lobate Flow Feature (LFF) on Mars (30˚-60˚ N&S hemispheres) to compare/assess the potentials of rock glaciers as an analog in suggesting LFFs to be a source of subsurface ice/water. LFFs are generally observed at the foot of impact craters' wall. HiRISE/CTX imageries from MRO spacecraft were used for geomorphological investigation of LFF using ArcMap-10.0 and subsurface investigation was carried out using data from MRO-SHARAD (shallow radar) after integrating with SiesWare-8.0. ENVI-5.0 was used to retrieve thermophysical properties of LFF from nighttime datasets (12.57 μm) acquired by THEMIS instrument-onboard the Mars Odyssey spacecraft and derive LFFs morphometry from MOLA altimeter point tracks onboard MGS spacecraft. Integrating crater chronology tool (Craterstats) with Arc Map, we have derived the formation age of LFF. Our investigation and comparison of LFF to rock glaciers revealed: (1) LFFs have preserved ice at depth ~50m as revealed from SHARAD radargram and top-layer composed of rocky-debris material with thermal inertia (~300-350 Jm -2 K -1 s -1/2 ).(2) LFF formation age (~10-100 Ma) corresponds to moderate scale debris covered glaciation of a shorter-span suggesting high sensitivity to obliquity-driven climatic shifts. (3) Presence of polygon cracks and high linear-arcuate furrow-and-ridges on the surface indicates presence of buried ice. This work is a significant step towards suggesting LFF to be a potential source of present-day stored ice/water on Mars.

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Amazonian modification of Moreux crater: Record of recent and episodic glaciation in the Protonilus Mensae region of Mars

Cited by 15 publications

References 92 publications

Possible polyphase periglaciation and glaciation adjacent to the Moreux impact-crater, Mars

Possible polyphase periglaciation and glaciation adjacent to the Moreux impact-crater, Mars

Former extent of glacier-like forms on Mars

Terrestrial rock glaciers: a potential analog for Martian lobate flow features (LFF)

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