PHASE-TRANSITIONS AND MELTING IN MARS

The basic thermal evolution model, described by Weizman et al. [1996], was modified to include the effect of phase transitions and the depen dence of melting temperatures on pressure. The total amount of mater r elease through Martian history was estimated from this model using: th e wet solidus of peridotite. Assuming a water content of 0.1% in the b asalt, we find that the total amount of water released would be suffic ient to cover the planet with a layer at least 3 - 300 m thick.