Recent formation and evolution of northern Martian polar layered deposits as inferred from a Global Climate Model

Details Recent formation and evolution of northern Martian polar layered deposits as inferred from a Global Climate Model Recent formation and evolution of northern Martian polar layered deposits as inferred from a Global Climate Model

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jgre..11206012l&link_type=abstract

Journal of Geophysical Research, Volume 112, Issue E6, CiteID E06012

Astronomy and Astrophysics

Astronomy

17

Planetary Sciences: Solid Surface Planets: Atmospheres (0343, 1060), Planetary Sciences: Solid Surface Planets: Orbital And Rotational Dynamics (1221), Planetary Sciences: Solid Surface Planets: Polar Regions, Planetary Sciences: Solid Surface Planets: Meteorology (3346), Planetary Sciences: Solar System Objects: Mars

Scientific paper

We present a time-marching model which simulates the exchange of water ice between the Martian northern cap, the tropics, and a high-latitude surface reservoir. Net annual exchange rates of water and their sensitivity to variations in orbital/rotational parameters are examined using the Martian water cycle modeled by the LMD three-dimensional Global Climate Model. These rates are propagated over the last 10 Myr to follow the thickness of the reservoirs. The effect of a sublimation dust lag is taken account to test simple models of layer formation. Periods of high mean polar summer insolation (~5-10 Ma ago) lead to a rapid exhaustion of a northern polar cap and a prolonged formation of tropical glaciers. The formation of a northern cap and of a high-latitude icy mantle may have started 4 Ma ago with the average decrease of polar insolation. Tropical ice may have disappeared around 2.7 Ma ago, but small glaciers could have formed during the last peaks of polar summer insolation. Over the last 4 Myr, most of the present cap may have formed at the expense of tropical and high-latitude reservoirs forming distinct layers at almost each ~51-kyr/120-kyr insolation cycle. Layers thickness ranges from 10 to 80 m, variations being produced by the modulation of the obliquity with ~2.4 and 1.3 Myr periods. Because only ~30 insolation cycles have occurred since 4 Ma ago, we found an inconsistency between the recent astronomical forcing, the observed number of layers, and simple astronomically based scenarios of layers formation.

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