The Effect Of Ground Ice Migration On The Martian Paleocarbon Dioxide Budget
E. David, O. Aharonson*, E. Vos, Weizmann Institute Of Science, Rehovot, Israel (Elad.David@Weizmann.Ac.Il),
*Also At: Planetary Science Institute, Tucson, Arizona, F. Forget, Laboratoire De Météorologie Dynamique, Jussieu, Paris, France.

Introduction:
The Mass And Distribution Of The Co2 And H2o
Ground Ice (Gi) Reservoirs On Mars Evolve In Response
To The Evolving Orbit Of Mars, Which Is Characterized
By Oscillations In Eccentricity (E), Longitude Of Perihelion (Lp) And Obliquity (Ε) [1]. The Seasonal Condensation/Sublimation Co2 Cycle Intensifies With Rising
Obliquity, As More Co2 Mass Exchanges Seasonally
Between Surface And Atmosphere; It Considerably Subdues As Obliquity Decreases, At Low Enough Obliquity
Reaching Atmospheric Collapse And The Formation Of
Massive Co2 Deposits [2,3]. Similarly, Ground Ice Extends Equatorward At High Obliquity, As Mid-Latitudes
Become More Humid And Receive Less Insolation, And
Recedes Back Poleward With Decreasing Obliquity
[4,5].
In Addition To The Individual Evolution Of The Two
Reservoirs, They Also Interact With Each Other: Due To
The High Thermal Conductivity Of Water Ice, Ground Ice
On Mars Acts As A Heat Sink During The Spring/Summer