Modeling of heat diffusion in magmatic dikes in the Martian crust

Abstract

The possibility that the Martian subsurface harbours liquid water is one of the central questions in the study of Mars’s habitability. In this context, the role of magmatic intrusions as a heat source capable of melting subsurface ice is studied. The heat diffusion equation is solved numerically using finite element simulation in COMSOL Multiphysics v6.4, modelling a saturated porous basaltic medium. The results show that a 50 m wide intrusion active for 100 years raises the 0°C isotherm to approximately 1405 m depth after 50 000 years. The sensitivity analysis reveals that the dike width is the dominant parameter, while the duration of the magmatism has a moderate effect and the thickness of the surface flow is practically irrelevant. The modelled timescales are consistent with recent volcanism at Cerberus Fossae, suggesting that similar episodes could have generated liquid water in the Martian subsurface