\begin{table}%T1
%\centering
\par
\caption{\label{TableSingleStars}Values of several stellar models. Nos.~1$-$3
are unevolved MS stars, 4 is a remnant of thermal timescale mass transfer
of an evolved MS star with an initial mass of \protect$ 1.5~ M_{\sun }\protect $,
an initial central hydrogen abundance of \protect$ 0.06\protect $,
an initially \protect$ 0.6~ M_{\sun }\protect $ white dwarf primary,
\protect$ \bar{\eta }=0.25\protect $, and subsequent mass loss
driven by strong braking according to  \citet{Verbunt-Zwaan}
using \protect$ f_{\rm {VZ}}=1\protect $. No.~5 is similar but
with an initial mass of \protect$ 3~ M_{\sun }\protect $, an initial
central hydrogen abundance of~\protect$ 0.41\protect $, an initially
\protect$ 1.4~ M_{\sun }\protect $ neutron star primary, and \protect$ \bar{\eta }\protect $
is determined by an Eddington accretion rate of \protect$ 2\times 10^{-8}~ M_{\sun }/\rm {yr}\protect $,
otherwise \protect$ \bar{\eta }=1\protect $. No.~6 is a giant.}
{\footnotesize \begin{tabular}{c|cccccc}
\hline \hline
Model No.&
1&
2&
3&
4&
5&
6\\
\hline
%\hline 
$ \vphantom {\sqrt{0}}X_{\rm {c}} $&
0.71&
0.71&
0.71&
0.05&
0.36&
0\\
%\hline 
$ \vphantom {\sqrt{0}}M_{2}/M_{\sun } $&
0.3&
0.5&
0.8&
0.45&
0.60&
0.8\\
%\hline 
$ \vphantom {\sqrt{0}}R_{2}/R_{\sun } $&
0.284&
0.436&
0.694&
0.695&
0.755&
25.81\\
%\hline 
$ \vphantom {\sqrt{0}}\log T_{0}/\rm {K} $&
3.552&
3.590&
3.705&
3.648&
3.738&
3.582\\
%\hline 
$ \vphantom {\sqrt{0}}\log L/L_{\sun } $&
--1.93&
--1.41&
--0.54&
--0.77&
--0.34&
2.10\\
%\hline 
$ \vphantom {\sqrt{0}}M_{\rm {ce}}/M_{2} $&
1.0&
0.23&
0.04&
0.17&
0.035&
0.63\\
%\hline 
$ \vphantom {\sqrt{0}}10^{4}H_{\rm {P}}/R_{2} $&
0.84&
1.00&
1.50&
2.2&
2.2&
41.1\\
%\hline 
$ \vphantom {\sqrt{0}}\zeta _{\rm {s}} $&
--0.31&
--0.08&
1.12&
0.60&
2.4&
0.14\\
%\hline 
$ \vphantom {\sqrt{0}}\zeta _{\rm {e}} $&
0.70&
1.04&
0.90&
0.76&
1.45&
--0.2\\
\hline
\end{tabular}}
\end{table}