Research Data

Reference

Animations

Figure 4/Figure 6: Evolution of disk surface density (solid blue line, left scale) and satellite mass (black dots, right scale) as a function of distance to Mars (semimajor axis in Mars radii). Simulation time is given at the top, and vertical dashed lines show the location of the rigid Roche Limit (1.74 Mars radii) and fluid Roche Limit (3.14 Mars radii). The simulation corresponds to a case with full destruction of Phobos, with initial disk mass being 1.1e4 masses of Phobos, particle size of 10 meters, and friction angle of 40 degrees.

Figure 11: Evolution of disk surface density (solid blue line, left scale) and satellite mass (black dots, right scale) as a function of distance to Mars (semimajor axis in Mars radii). Simulation time is given at the top, and vertical dashed lines show the location of the rigid Roche Limit (1.74 Mars radii) and fluid Roche Limit (3.14 Mars radii). The simulation corresponds to a case with full destruction of Phobos and including Yarkovsky effects, with initial disk mass being 0.9e4 masses of Phobos, particle size of 0.1 meters, and friction angle of 25 degrees.

Figure 13: Evolution of disk surface density (solid blue line, left scale) and satellite mass (black dots, right scale) as a function of distance to Mars (semimajor axis in Mars radii). Simulation time is given at the top, and vertical dashed lines show the location of the rigid Roche Limit (1.74 Mars radii) and fluid Roche Limit (3.14 Mars radii). The simulation corresponds to a case with tidal downsizing, with initial disk mass being 1.1e4 masses of Phobos, particle size of 10 meters, and friction angle of 40 degrees.