Hot subdwarfs from the stable Roche lobe overflow channel

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Table 4:

Birth rates of hot subdwarfs from the stable RLOF channel of intermediate-mass binaries (our model) and other channels (Han et al. 2003) (in 10^-3 yr^-1).
Z	$q_{\rm crit}$	$\nu_{\rm IMR}$	$\nu_{\rm FR}$	$\nu_{\rm FCE}$	$\nu_{\rm SR}$	$\nu_{\rm SCE}$	$\nu_{\rm M}$
0.02	1.5	4.18	29.89	8.41	0.00	8.38	17.22
0.02	1.2	4.14	22.25	10.71	0.00	5.43	7.99

Z = metallicity; $q_{\rm crit}$ = the critical mass ratio for the first stable RLOF on the FGB; $\nu_{\rm IMR}$ = Galactic birth rates of hot subdwarfs from the stable RLOF channel of intermediate-mass binaries; $\nu_{\rm FR}$ = the first stable RLOF channel; $\nu_{\rm FCE}$ = the first CE ejection channel; $\nu_{\rm SR}$ = the second RLOF channel; $\nu_{\rm SCE}$ = the second CE ejection channel; $\nu_{\rm M}$ = the helium WD merger channel.

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