Dynamics of a fluid flow on Mars: Lava or mud?

Abstract

A distinctive flow deposit southwest of Cerberus Fossae on Mars is analyzed. The flow source is a ∼20m deep, ∼12×1.5km wide depression within a yardang associated with the Medusae Fossae Formation. The flow traveled for ∼40km following topographic lows to leave a deposit on average 3–4km wide. The surface morphology of the deposit suggests that it was produced by the emplacement of a fluid flowing in a laminar fashion and possessing a finite yield strength. We use topographic data from a digital elevation model (DEM) to model the dynamics of the motion and infer that the fluid had a Bingham rheology with a plastic viscosity of ∼1Pas and a yield strength of ∼185Pa. Although the low viscosity is consistent with the properties of komatiite-like lava, the combination of values of viscosity and yield strength, as well as the surface morphology of the flow, suggests that this was a mud flow. Comparison with published experimental data implies a solids content close to 60% by volume and a grain size dominated by silt-size particles. Comparison of the ∼1.5km3 deposit volume with the ∼0.03km3 volume of the source depression implies that ∼98% of the flow material was derived from depth in the crust. There are similarities between the deposit studied here, which we infer to be mud, and other flow deposits on Mars currently widely held to be lavas. This suggests that a re-appraisal of many of these deposits is now in order.