The mass range of hot subdwarf B stars from MESA simulations

0585410 - ASÚ 2025 RIV US eng J - Journal Article
Arancibia-Rojas, E. - Zorotovic, M. - Vučković, M. - Bobrick, A. - Vos, Joris - Piraino-Cerda, F.
The mass range of hot subdwarf B stars from MESA simulations.
Monthly Notices of the Royal Astronomical Society. Roč. 257, č. 4 (2024), , , 1184-11197-1197. ISSN 0035-8711. E-ISSN 1365-2966
R&D Projects: GA ČR(CZ) GA22-34467S
Institutional support: RVO:67985815
Keywords : binaries: general * stars: evolution * stars: mass-loss
OECD category: Astronomy (including astrophysics,space science)
Impact factor: 4.8, year: 2022
Method of publishing: Open access

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 ~2.0 M⊙. For stars more massive than ~2.5 M⊙, 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.
Permanent Link: https://hdl.handle.net/11104/0353119