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It is expected since the early 1970s that tenuous dust rings are formed bygrains ejected from the Martian moons Phobos and Deimos by impacts ofhypervelocity interplanetary projectiles. In this paper, we perform directnumerical integrations of a large number of dust particles originating fromPhobos and Deimos. In the numerical simulations, the most relevant forcesacting on dust are included: Martian gravity with spherical harmonics up to 5thdegree and 5th order, gravitational perturbations from the Sun, Phobos, andDeimos, solar radiation pressure, as well as the Poynting-Robertson drag. Inorder to obtain the ring configuration, simulation results of various grainsizes ranging from submicron to 100 microns are averaged over a specifiedinitial mass distribution of ejecta. We find that for the Phobos ring grainssmaller than about 2 microns are dominant; while the Deimos ring is dominatedby dust in the size range of about 5-20 microns. The asymmetries, numberdensities and geometrical optical depths of the rings are quantified fromsimulations. The results are compared with the upper limits of the opticaldepth inferred from Hubble observations. We compare to previous work anddiscuss the uncertainties of the models.

Configuration of the Martian dust rings: Shapes, densities and size-distributions from direct integrations of particle trajectories