Distribution of Hydrogen in the Near Surface of Mars: Evidence for Subsurface Ice Deposits

Boynton, W. V.; Feldman, W. C.; Squyres, S. W.; Prettyman, T. H.; Brückner, J.; Evans, L. G.; Reedy, R. C.; Starr, R.; Arnold, J. R.; Drake, D. M.; Englert, P.; Metzger, A. E.; Митрофанов, И. Г.; Trombka, J. I.; d’Uston, C.; Wänke, H.; Gasnault, O.; Hamara, D.; Janes, D. M.; Marcialis, R. L.; Maurice, S.; Mikheeva, I. B.; Taylor, G. J.; Tokar, R. L.; Shinohara, C.

doi:10.1126/science.1073722

Cited by 880 publications

(518 citation statements)

References 14 publications

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“…Theoretical simulations performed by many authors (Leighton and Murray, 1966;Fanale et al, 1986;Mellon and Jakosky, 1995;Schorghofer and Aharonson, 2005;Aharonson and Schorghofer, 2006) led finally to the conclusion, that the subsurface ice may be present in wide range of latitudes. The neutron and gamma ray spectrometers on board Mars Odyssey spacecraft confirmed, that some subsurface ice is present almost everywhere on Mars except low latitudes (Boynton et al, 2002;Mitrofanov et al, 2004). This is in agreement with other observations (Kossacki et al, 2003;Titus et al, 2003).…”

Section: Introductionsupporting

confidence: 90%

Small-scale trench in the north polar region of Mars: Evolution of surface frost and ground ice concentration

Kossacki¹,

Markiewicz²

2009

Icarus

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In this paper we attempt to answer the question, how formation of a small-scale trench in the Martian regolith affects local distribution of the subsurface ice. We are especially interested in the consequences of digging a trench to search for buried ice, as has been done during the Phoenix Mars Lander mission. However, the results may be also applicable for natural troughs, or cracks. We present results of simulations of diurnal exchange of water between the regolith and the atmosphere. Our model includes the heat and vapor migration in the regolith surrounding the trench, as well as formation of diurnal frost. We take into account scattering of light in the atmosphere and on the trench facets, as well as changes of atmospheric humidity on diurnal and seasonal time scales. Our calculations show, that the measurements of ice content in a sample obtained within one, or two days from the beginning of digging should not be affected. However, on somewhat longer time scale at the south facing site of the trench the regolith can be significantly depleted from ice. This effect should be taken into account if the excavation and taking samples from different depths will be performed in stages separated in time by a month, or more.

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Section: Introductionsupporting

confidence: 90%

Small-scale trench in the north polar region of Mars: Evolution of surface frost and ground ice concentration

Kossacki¹,

Markiewicz²

2009

Icarus

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“…These theoretical expectations appear consistent with measurements of the near-surface (top ∼0.5 m) regolith hydrogen abundance made by the Mars Odyssey Gamma Ray Spectrometer (GRS) (Boynton et al, 2002;Feldman et al, 2002). The GRS data are usually interpreted in the context of a simple 2-layer model, wherein ice-rich (>60% by volume) regolith is assumed to underlie a desiccated layer of variable thickness.…”

Section: What Is the Current Distribution Of Exchangeable Reservoirs supporting

confidence: 73%

Introduction to the 4th Mars Polar Science and Exploration Conference special issue: Five top questions in Mars polar science

Fishbaugh

Hvidberg

Beaty

et al. 2008

Icarus

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“…Gamma Ray Spectrometer and Neutron Spectrometer (GRS/NS) observations of regolith at latitudes N50-60°show substantial amounts of water ice within a few tens of centimeters of the surface (Boynton et al, 2002;Feldman et al, 2004). The soils may therefore have had a degree of cohesion from ice cement holding the grains together, resulting in little mobile sediment available for transport by the wind.…”

Section: Sediment Source and Spatial Distributionmentioning

confidence: 99%

Transverse Aeolian Ridges (TARs) on Mars

et al. 2008

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Aeolian processes are probably the dominant ongoing surface process on Mars; Large Dark Dunes (LDDs), particularly common aeolian landforms, were first recognized in the early 1970s. Recent, higher resolution images have revealed another, morphologically distinct, large population of smaller, ripple-like aeolian bedforms that have been termed "Transverse Aeolian Ridges" (TARs) as it is unknown whether they formed as large ripples or small dunes. We have begun a new study of TARs that examines their distribution, orientation, and morphology using N 10,000 high-resolution Mars Orbiter Camera (1.5 to 8 m/pixel resolution) images in a 45°longitude wide, pole-to-pole survey. The aim of this study is to assess whether TARs are active, to identify possible sediment sources and pathways, and to determine the volumes of sediment that they comprise. We present results from the first half of this study, in which we examine the northern hemisphere, and describe a new three-part classification scheme used to aid the survey. Our results show that TARs are abundant but not ubiquitous: preferentially forming proximal to friable, layered terrains such as those found in Terra Meridiani -the location of the ongoing Mars Exploration Rover "Opportunity" mission. TAR distribution in the northern hemisphere shows a strong latitudinal dependence with very few TARs being found north of ∼ 30°N. We also find that in most cases TARs are less mobile than LDDs, a conclusion possibly explained by Mars Exploration Rover Opportunity observations that show TARlike ripples to have a core of fine material armored by a monolayer of granule-sized particles. This could disallow significant bedform movement under the current wind regime. That TARs are essentially inactive is confirmed by superposition relations with slope streaks and LDDs and by observations of superposed impact craters. We suggest that observations made by the Opportunity Rover in Terra Meridiani indicate that the small aeolian bedforms common here are ripples and not small dunes. Farther south, these bedforms transition into larger features indistinguishable from TARs, suggesting that TARs (in the Meridiani area at least) are ripples and not dunes.

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Distribution of Hydrogen in the Near Surface of Mars: Evidence for Subsurface Ice Deposits

Cited by 880 publications

References 14 publications

Small-scale trench in the north polar region of Mars: Evolution of surface frost and ground ice concentration

Small-scale trench in the north polar region of Mars: Evolution of surface frost and ground ice concentration

Introduction to the 4th Mars Polar Science and Exploration Conference special issue: Five top questions in Mars polar science

Transverse Aeolian Ridges (TARs) on Mars

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