  Hot subdwarf B (sdB) stars are helium core burning stars that have lost
almost their entire hydrogen envelope due to binary interaction. Their assumed
canonical mass of $\rm M_{\mathrm{sdB}}\sim0.47 M_{\odot}$ has recently been
debated given a broad range found both from observations as well as from the
simulations. Here, we revise and refine the mass range for sdBs derived two
decades ago with the Eggleton code, using the stellar evolution code MESA, and
discuss the effects of metallicity and the inclusion of core overshooting
during the main sequence. We find an excellent agreement for low-mass
progenitors, up to $\sim2.0 \rm M_{\odot}$. For stars more massive than
$\sim2.5 \rm M_{\odot}$ we obtain a wider range of sdB masses compared to the
simulations from the literature. Our MESA models for the lower metallicity
predict, on average, slightly more massive sdBs. Finally, we show the results
for the sdB lifetime as a function of sdB mass and discuss the effect this
might have in the comparison between simulations and observational samples.
This study paves the way for reproducing the observed Galactic mass
distribution of sdB binaries.
