Distribution of Mid-Latitude Ground Ice on Mars from New Impact Craters

Byrne, Shane; Dundas, C. M.; Kennedy, M. R.; Mellon, M. T.; McEwen, A. S.; Cull, Selby; Daubar, I. J.; Shean, David; Seelos, K. D.; Murchie, S. L.; Cantor, B. A.; Arvidson, R. E.; Edgett, K. S.; Reufer, A.; Thomas, N.; Harrison, Tanya N.; Posiolova, Liliya; Seelos, F. P.

doi:10.1126/science.1175307

Cited by 287 publications

(219 citation statements)

References 34 publications

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“…However, the presence of water ice in the shallow subsurface midlatitude and polar regions Mitrofanov et al 2002;Byrne et al 2009), along with the detection of perchlorates in polar and equatorial soil Glavin et al 2013;Ming et al 2014) and of chloride-bearing deposits in the southern highlands at low and midlatitudes (Osterloo et al 2008), is important because they can melt this ice at Mars' present-day environmental conditions and produce liquid saline water (brine) (Clark 1978;Brass 1980;Clark and Van Hart 1981;Haberle et al 2001;Chevrier and Altheide 2008;Rennó et al 2009;McEwen et al 2011;Ojha et al 2015).…”

Section: Liquid Water and The H 2 O Cyclementioning

confidence: 99%

The Modern Near-Surface Martian Climate: A Review of In-situ Meteorological Data from Viking to Curiosity

et al. 2017

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We analyze the complete set of in-situ meteorological data obtained from the Viking landers in the 1970s to today's Curiosity rover to review our understanding of the modern near-surface climate of Mars, with focus on the dust, CO 2 and H 2 O cycles and their impact on the radiative and thermodynamic conditions near the surface. In particular, we provide values of the highest confidence possible for atmospheric opacity, atmospheric pressure, near-surface air temperature, ground temperature, near-surface wind speed and direction, and near-surface air relative humidity and water vapor content. Then, we study the diurnal, seasonal and interannual variability of these quantities over a span of more thanThe original version of this article was revised because due to an unfortunate turn of events a wrong value was published in Table 1. The resolution of the PHX pressure sensor was published as "0.1 mbar" whereas this value has now been corrected to "0.1 Pa" which is the correct value and should be regarded as the final version by the reader. B G.M. Martínez

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Section: Liquid Water and The H 2 O Cyclementioning

confidence: 99%

The Modern Near-Surface Martian Climate: A Review of In-situ Meteorological Data from Viking to Curiosity

et al. 2017

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“…Earth-style cementation (i.e., lithification), which typically occurs in the subsurface with the passage of large volumes of pore waters, must be very restricted on Mars because of the waterlimited state. Rather, Martian strata are probably poorly lithified, and ice/frost cementation is widespread (e.g., Schatz et al 2006, Byrne et al 2009). Given ice cementation, sediment generation (recycling) would occur with sublimation driven by climatic cycles at a variety of temporal scales (i.e., daily to Milankovitch).…”

Section: Marsmentioning

confidence: 99%

Source-to-Sink

Kocurek¹,

Ewing²

2012

Sedimentary Geology of Mars

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Eolian dune fields on Earth and Mars evolve as complex systems within a set of boundary conditions. A source-to-sink comparison indicates that although differences exist in sediment production and transport, the systems largely converge at the dune-flow and pattern-development levels, but again differ in modes of accumulation and preservation. On Earth, where winds frequently exceed threshold speeds, dune fields are sourced primarily through deflation of subaqueous deposits as these sediments become available for transport. Limited weathering, widespread permafrost, and the lowdensity atmosphere on Mars imply that sediment production, sediment availability, and sand-transporting winds are all episodic. Possible sediment sources include relict sediments from the wetter Noachian; slow physical weathering in a cold, water-limited environment; and episodic sediment production associated with climatic cycles, outflow events, and impacts. Similarities in dune morphology, secondary airflow patterns over the dunes, and pattern evolution through dune interactions imply that dune stratification and bounding surfaces on Mars are comparable to those on Earth, an observation supported by outcrops of the Burns formation. The accumulation of eolian deposits occurs on Earth through the dynamics of dry, wet, and stabilizing eolian systems. Dry-system accumulation by flow deceleration into topographic basins has occurred throughout Martian history, whereas wetsystem accumulation with a rising capillary fringe is restricted to Noachian times. The greatest difference in accumulation occurs with stabilizing systems, as manifested by the north polar Planum Boreum cavi unit, where accumulation has occurred through stabilization by permafrost development. Preservation of eolian accumulations on Earth typically occurs by sediment burial within subsiding basins or a relative rise of the water table or sea level. Preservation on Mars, measured as the generation of a stratigraphic record and not time, has an Earth analog with infill of impact-created and other basins, but differs with the cavi unit, where preservation is by burial beneath layered ice with a climatic driver.

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“…We refer the reader to Daubar and McEwen (2009), Daubar et al (2010Daubar et al ( , 2011a, Ivanov et al (2008Ivanov et al ( , 2009), Kennedy and Malin (2009), Byrne et al (2009), and McEwen et al (2007a,b, 2010 for further information on these new impact sites.…”

Section: Introductionmentioning

confidence: 99%