Comparison of the evolutionary tracks of LMXBs with and without evaporation in the ﹩{M}_{2}\mbox{--}{P}_{\mathrm{orb}}﹩ plane. The solid, dot-dashed, and dotted lines correspond to the standard model (f = 0) and the models of Mode A and B evaporation (f = 0.1), respectively. The open circles and squares indicate the birth of proto-WDs and the beginning of their cooling phase, respectively. All the calculations are ended at Hubble age, except for the tracks ended with crosses, which represent the start of runaway mass transfer. The initial secondary mass is 1 M_⊙, and the initial periods for each group are 3.2, 2.9, 2.75, 2.4, and 0.5 days. The thin solid line represents the theoretical ﹩{M}_{\mathrm{WD}}\mbox{--}{P}_{\mathrm{orb}}﹩ relation given by Lin et al. (2011) for Pop I stars.