Mars at very low obliquity: Atmospheric collapse and the fate of volatiles

Details Mars at very low obliquity: Atmospheric collapse and the fate of volatiles Mars at very low obliquity: Atmospheric collapse and the fate of volatiles

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005georl..3212202k&link_type=abstract

Geophysical Research Letters, Volume 32, Issue 12, CiteID L12202

Mathematics

Logic

11

Planetary Sciences: Solid Surface Planets: Polar Regions, Planetary Sciences: Solid Surface Planets: Orbital And Rotational Dynamics (1221), Planetary Sciences: Solid Surface Planets: Glaciation, Planetary Sciences: Solid Surface Planets: Atmospheres (0343, 1060), Planetary Sciences: Solar System Objects: Mars

Scientific paper

The obliquity of the Martian spin axis is known to undergo quasiperiodic oscillations superposed over chaotic long-term variations. It is probable that within past history there were geologically long periods when the obliquity oscillated around low (10-15°) mean values. During such low obliquity epochs the climate system is controlled by deposition of permanent solid CO2 deposits in the polar regions. With a simple season-resolved energy balance model, we show that as the atmosphere collapses, surface topography plays a major role in CO2 condensation and sublimation processes, defining distribution and dynamics of CO2 deposits. Thick CO2 deposits are formed at steep pole-facing topographic slopes at moderately high latitudes, not at the poles. The total mass of the deposits is not a function of obliquity, but strongly depends on the pre-history of the climate system. We outline criteria to identify such low-obliquity epochs in Mars history.

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