Characteristic debris size as a function of astrocentric distance and minimum cohesive strength. We assume a 0.6 M_⊙ mass white dwarf. The bottom panels are zoomed-in versions of the top panels. For minimum cohesive strengths of (left panels) 10 Pa and (right panels) 1 kPa, we find characteristic sizes on the order of ∼100 and ∼1000 m, respectively. Although the density of a material can strongly influence disruption behavior, the densities of real planetary materials typically tidally disrupt into debris with these characteristic sizes.