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Instability of ice at low-latitudes leads to sublimation and cold-trapping at the poles
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Classroom Contents
The Climatic and Hydrologic Evolution of Water on Mars
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- 1 Intro
- 2 Why We Care About Water On Mars
- 3 Estimated Martian Inventory of H2O
- 4 Martian Global Inventory of H2O: -0.5 - 1 km GEL, 2 -3.5 Ga (Carr, 1986)
- 5 Early Mars: Warm or Cold?
- 6 Potential Evolution of the Martian Hydrosphere
- 7 Mars Thermal History Model: Mantle Heat Flow vs. Time 400
- 8 Nature of the Martian Crust
- 9 Gravitationally-Scaled, Globally-Averaged Porosity & Permeability Profiles for Mars
- 10 Crater with Fluidized Ejecta: Potential Indicators of Impacts into a Water-or Ice-Rich Crust
- 11 Inferred hydraulic conditions by Late Hesperian, implied by elevation of outflow channel source regions: North
- 12 Hydraulic conditions during Late Hesperian
- 13 Inferred hydraulic conditions during the Noachian 3.8 Gya after the onset of a colder climate
- 14 Geomorphic Identification of Potential Paleoshorelines in the Martian Northern Plains (Parker et al., 1987, 1989, 1993; Clifford and Parker, 2001; Parker et al., 2010)
- 15 Distribution of Valley Networks Most Readily Explained by the Existence of a Martian Northern Ocean (Soto et al., 2010)
- 16 Instability of ice at low-latitudes leads to sublimation and cold-trapping at the poles
- 17 Potential Recharge of Subpermafrost Groundwater by Polar Basal Melting
- 18 Geomorphic Evidence of Hesperian-Age Polar Basal Melting: Eskers, Valleys and the Chryse Trough Drainage System
- 19 Ocean freezes and cryosphere thickens, permitting rise of global water table
