The presence and stability of ground ice in the southern hemisphere of Mars

By M. Mellon, W. Feldman, T. Prettyman. 2004

359 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/98e8f2f627b4e9179b81cee8d9ae33913f266518

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Citations in the corpus

Widespread excess ice in Arcadia Planitia, Mars (2015, background): “Models of the distribution of ice stability with the current Martian climate (and today’s lower-than-average obliquity) suggest that water ice should be stable poleward of the midlatitudes (~40–50°) within a meter of the surface and stable closer to the surface near the poles [Mellon et al., 2004; S”
Apparent thermal inertia and the surface heterogeneity of Mars (2007, methodology): “…of ground-ice stability in the polar regions as well as at lower latitudes (Paige, 1992; Mellon and Jakosky, 1993, 1995; Vasavada et al., 2000; Mellon et al., 2004) and the recent detection of near-surface hydrogen attributed to the presence of ground ice (Boynton et al., 2002; Feldman et…”
Hydration state of the Martian surface as seen by Mars Express OMEGA: 2. H2O content of the surface (2007, methodology): “various hydration states of palagonite in Figure 1a (see Milliken and Mustard [2007a] for a detailed analysis of low-albedo hydrated materials).”
The High Resolution Imaging Science Experiment (HiRISE) during MRO’s Primary Science Phase (PSP) (2010, background): “, 2004) and the theoretically predicted geographic distribution of ground-ice stability (Mellon and Jakosky, 1993; Mellon et al., 2004) suggests that the margin of currently present, yet unstable ice is roughly coincident with the latitudinal band characterized by erosional features.”
Possible physical and thermodynamical evidence for liquid water at the Phoenix landing site (2009, background): “5.1. Spheroids Growth by Deliquescence [18] A lower bound to the temperature of the ice exposed under the lander is about 200–210 K [ Mellon et al., 2004 ].”
Formation of recurring slope lineae by liquid brines on present‐day Mars (2012, background): “…can accurately reproduce several RSL key characteristics (e.g. preference for equator-facing slopes and observed seasonality), it requires the presence of buried ice within the regolith column, which in the southern hemisphere is only considered stable for latitudes >40 S [Mellon et al., 2004].”
NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance (2018, background): “However, subsurface ice (Mellon et al. 2004, 2009) may also be a source of atmospheric water, possibly with a different D/H ratio.”
Stability and exchange of subsurface ice on Mars (2005, methodology): “, 2004] that can be compared with predictions of an equilibrium ice table [Boynton et al., 2002; Mellon et al., 2004].”
Ground ice at the Phoenix Landing Site: Stability state and origin (2009, methodology): “and diffusive equilibrium [see also Mellon et al., 2004 ].”
Global thermal inertia and surface properties of Mars from the MGS mapping mission (2005, background): “In the upper few centimeters (the T sensing depth), ice is seasonally unstable even at high tudes and the regolith is expected to desiccate(M llon and Jakosky, 1995; Mellon et al., 2004).”
SHARAD sounding radar on the Mars Reconnaissance Orbiter (2007, background): “While the depths to the top of the ice (typically Mellon et al., 2004 ], depths to the bottom of the ice are poorly known.”
Thermal contraction crack polygons on Mars: Classification, distribution, and climate implications from HiRISE observations (2009, result): “…latitude distribution is consistent with models predicting the distribution of sufficient ground ice to cement permafrost [Mellon and Jakosky, 1995; Mellon et al., 2004], as well as models predicting the distribution of seasonal thermal stresses sufficient to generate thermal contraction cracking…”