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gfdl's home page > gfdl on-line bibliography > 2003: Journal of Geophysical Research, 108(E6), 5062, doi:10.1029/2003JE002051

On the orbital forcing of Martian water and CO2 cycles: A general circulation model study with simplified volatile schemes

Mischna, M., M. I. Richardson, R. J. Wilson, and D. J. McCleese, 2003: On the orbital forcing of Martian water and CO₂ cycles: A general circulation model study with simplified volatile schemes. Journal of Geophysical Research, 108(E6), 5062, doi:10.1029/2003JE002051.

Abstract: Variations in the Martian water and CO₂ cycles with changes in orbital and rotational parameters are examined using the Geophysical Fluid Dynamics Laboratory Mars General Circulation Model. The model allows for arbitrary specification of obliquity, eccentricity, and argument of perihelion as well as the position and thickness of surface ice. Exchange of CO₂ between the surface and atmosphere is modeled, generating seasonal cycles of surface ice and surface pressure. Water is allowed to exchange between the surface and atmosphere, cloud formation is treated, and both cloud and vapor are transported by modeled winds and diffusion. Exchange of water and CO₂ with the subsurface is not allowed, and radiative effects of water vapor and clouds are not treated. The seasonal cycle of CO₂ is found to become more extreme at high obliquity, as suggested by simple heat balance models. Maximum pressures remain largely the same, but the minima decrease substantially as more CO₂ condenses in the more extensive polar night. Vapor and cloud abundances increase dramatically with obliquity. The stable location for surface ice moves equatorward with increasing obliquity, such that by 45° obliquity, water ice is stable in the tropics only. Ice is not spatially uniform, but rather found preferentially in regions of high thermal inertia or high topography. Eccentricity and argument of perihelion can provide a second-order modification to the distribution of surface ice by altering the temporal distribution of insolation at the poles. Further model simulations reveal the robustness of these distributions for a variety of initial conditions. Our findings shed light on the nature of near-surface, ice-rich deposits at midlatitudes and low-latitudes on Mars.

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