All Tables

Table 1: Values of several stellar models. Nos. 1-3 are unevolved MS stars, 4 is a remnant of thermal timescale mass transfer of an evolved MS star with an initial mass of $1.5~ M_{\hbox{$\odot$ }}\protect$ , an initial central hydrogen abundance of $0.06\protect$ , an initially $0.6~ M_{\hbox{$\odot$ }}\protect$ white dwarf primary, $\bar{\eta }=0.25\protect$ , and subsequent mass loss driven by strong braking according to Verbunt & Zwaan (1981) using $f_{\rm {VZ}}=1\protect$ . No. 5 is similar but with an initial mass of $3~ M_{\hbox{$\odot$ }}\protect$ , an initial central hydrogen abundance of $0.41\protect$ , an initially $1.4~ M_{\hbox{$\odot$ }}\protect$ neutron star primary, and $\bar{\eta }\protect$ is determined by an Eddington accretion rate of $2\times 10^{-8}~ M_{\hbox{$\odot$ }}/\rm {yr}\protect$ , otherwise $\bar{\eta }=1\protect$ . No. 6 is a giant.
Table 2: System parameters of CVs containing an $0.5~ M_{\hbox{$\odot$ }}\protect$ donor as shown in Fig. 9.