Evolution of CVs below the period gap. The solid lines show the tracks on the M₂ − P_orb plane (lower x- and left y-axis). The dashed tracks in the M₂ − B plane (lower x- and right y-axis) show the evolution of B (Eq. (1)) for the models in which κ depends on stellar parameters. The ticks on each solid track denote timesteps of 300 Myr. The different colors correspond to different κs. The grey points are CVs reported by Knigge (2006, their Table 1). We also plot observed period bouncer candidates from Table B.1. Eclipsing systems are plotted as circles, while non-eclipsing systems are plotted as triangles. The horizontal shaded region is the observed period minimum spike (80 ≲ P_orb/min ≲ 86) reported by Gänsicke et al. (2009). The squares of different colors show when the system has Ṁ₂ = 10⁻¹¹ M_⊙ yr⁻¹. During further evolution, the system is presumably undetectable (see text).