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.
Model No. 1 2 3 4 5 6

$\vphantom {\sqrt{0}}X_{\rm {c}}$ 0.71 0.71 0.71 0.05 0.36 0

$\vphantom {\sqrt{0}}M_{2}/M_{\hbox{$\odot$ }}$ 0.3 0.5 0.8 0.45 0.60 0.8

$\vphantom {\sqrt{0}}R_{2}/R_{\hbox{$\odot$ }}$ 0.284 0.436 0.694 0.695 0.755 25.81

$\vphantom {\sqrt{0}}\log T_{0}/\rm {K}$ 3.552 3.590 3.705 3.648 3.738 3.582

$\vphantom {\sqrt{0}}\log L/L_{\hbox{$\odot$ }}$ -1.93 -1.41 -0.54 -0.77 -0.34 2.10

$\vphantom {\sqrt{0}}M_{\rm {ce}}/M_{2}$ 1.0 0.23 0.04 0.17 0.035 0.63

$\vphantom {\sqrt{0}}10^{4}H_{\rm {P}}/R_{2}$ 0.84 1.00 1.50 2.2 2.2 41.1

$\vphantom {\sqrt{0}}\zeta _{\rm {s}}$ -0.31 -0.08 1.12 0.60 2.4 0.14

$\vphantom {\sqrt{0}}\zeta _{\rm {e}}$ 0.70 1.04 0.90 0.76 1.45 -0.2

**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.
Model No.	1	2	3	4	5	6
$\vphantom {\sqrt{0}}X_{\rm {c}}$	0.71	0.71	0.71	0.05	0.36	0
$\vphantom {\sqrt{0}}M_{2}/M_{\hbox{$\odot$ }}$	0.3	0.5	0.8	0.45	0.60	0.8
$\vphantom {\sqrt{0}}R_{2}/R_{\hbox{$\odot$ }}$	0.284	0.436	0.694	0.695	0.755	25.81
$\vphantom {\sqrt{0}}\log T_{0}/\rm {K}$	3.552	3.590	3.705	3.648	3.738	3.582
$\vphantom {\sqrt{0}}\log L/L_{\hbox{$\odot$ }}$	-1.93	-1.41	-0.54	-0.77	-0.34	2.10
$\vphantom {\sqrt{0}}M_{\rm {ce}}/M_{2}$	1.0	0.23	0.04	0.17	0.035	0.63
$\vphantom {\sqrt{0}}10^{4}H_{\rm {P}}/R_{2}$	0.84	1.00	1.50	2.2	2.2	41.1
$\vphantom {\sqrt{0}}\zeta _{\rm {s}}$	-0.31	-0.08	1.12	0.60	2.4	0.14
$\vphantom {\sqrt{0}}\zeta _{\rm {e}}$	0.70	1.04	0.90	0.76	1.45	-0.2

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