Figure 3:
Relationship between white dwarf temperature and sublimation radius for forsterite, fayalite, iron, and enstatite. We compute the radius of transition from radiative to sublimative cooling (the sublimation radius), and thus the inner edge of a dusty debris disk, as a function of white dwarf temperature for these four species for the most probable white dwarf mass (0.6 Msolar), and the most probable range of white dwarf masses (0.5 and 0.7 Msolar). Dashed and dash-dotted lines denote the rigid body Roche limit for densities of 3500 and 2000 kg/m3 respectively.