Heat flow perturbations from isolated rock bodies in the Martian regolith

Abstract

One of the key quantities for accessing the present thermal state of a planet is measuring its planetary heat flow. It yields information about tectonic and magmatic processes and is essential to resolve the thermal evolution. Upcoming in situ measurements are designed to log the temperature and thermal conductivity in the upper 5 m of the Martian regolith. In a previous study it was shown that a determination of the planetary heat flow is feasible if the annual mean temperatures in the subsurface can be determined by, e.g., extending the measurement period over at least a full Martian year. So far, modelling has been done for a homogeneous fine- or coarse-grained regolith without regarding isolated rock or ice bodies within the regolith which are expected to disturb the heat flow seriously. A 2D numerical modelling approach gives a first impression of how heterogeneities could affect temperature logging and planetary heat flow. For the simulations we have used material properties that correspond to those of similar terrestrial rock.