The mass range of hot subdwarf B stars from MESA simulations

0585410 - ASÚ 2025 RIV US eng J - Článek v odborném periodiku
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
Grant CEP: GA ČR(CZ) GA22-34467S
Institucionální podpora: RVO:67985815
Klíčová slova: binaries: general * stars: evolution * stars: mass-loss
Obor OECD: Astronomy (including astrophysics,space science)
Impakt faktor: 4.8, rok: 2022
Způsob publikování: 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.
Trvalý link: https://hdl.handle.net/11104/0353119