Possible core evolutionary states for Mars have been recently summarized [Stevenson, 2001]. We will assess the convective stability of these models by performing a suite of numerical experiments using a model developed by Bloxham [Kuang and Bloxham, 1999] that treats magnetohydrodynamic convective flow of a Boussinesq fluid in a rapidly rotating spherical shell. We expect this modeling to provide guidance relating to physical core conditions consistent with a main magnetic field. Ultimately it will be necessary to perform a more rigorous assessment of the potential for dynamo action, that will require a serious study of forces and dissipation mechanisms [Glatzmaier and Roberts, 1996; Kuang and Bloxham, 1997].
REFERENCES
Glatzmaier, G., and P.H. Roberts, Rotation and magnetism of Earth's inner core, Science, 274, 1887-1890, 1996.
Kuang, W., and J. Bloxham, A numerical model of the generation of the Earth's magnetic field, Nature, 365, 371-374, 1997.
Kuang, W., and J. Bloxham, Numerical modeling of magnetohydrodynamic convection in a rapidly rotating spherical shell: Weak and strong field dynamo action, J. Comp. Phys., 153, 51-81, 1999.
Stevenson, D.J., Mars' core and magnetism, Nature, 412, 214-219, 2001.