Grids of stellar models with rotation

Article Article scientifique Article Grids of stellar models with rotation eng 2021-08-24 2021-08-24 author Eggenberger Patrick 0000-0001-6319-9297 504578 author Ekström Sylvia 0000-0002-2564-5660 514725 author Georgy Cyril 0000-0003-2362-4089 540258 author Martinet Sébastien 0000-0001-5411-5098 910315 author Pezzotti Camilla 910356 author Nandal Devesh 935095 author Meynet Georges 22422 author Buldgen Gaël 909685 author Salmon Sébastien 936024 author Haemmerle Lionel 582194 author Maeder André 25143 author Hirschi Raphael 527684 author Yusof Norhasliza author Groh José 779776 author Farrell Eoin author Murphy Laura author Choplin Arthur 828201 A137 10.1051/0004-6361/202141222 0004-6361 https://www.aanda.org/10.1051/0004-6361/202141222 Context. Grids of stellar models, computed with the same physical ingredients, allow one to study the impact of a given physics on a broad range of initial conditions and they are a key ingredient for modeling the evolution of galaxies. Aims. We present here a grid of single star models for masses between 0.8 and 120 M ⊙ , with and without rotation for a mass fraction of heavy element Z = 0.006, representative of the Large Magellanic Cloud (LMC). Methods. We used the GENeva stellar Evolution Code. The evolution was computed until the end of the central carbon-burning phase, the early asymptotic giant branch phase, or the core helium-flash for massive, intermediate, and low mass stars, respectively. Results. The outputs of the present stellar models are well framed by the outputs of the two grids obtained by our group for metallicities above and below the one considered here. The models of the present work provide a good fit to the nitrogen surface enrichments observed during the main sequence for stars in the LMC with initial masses around 15 M ⊙ . They also reproduce the slope of the luminosity function of red supergiants of the LMC well, which is a feature that is sensitive to the time-averaged mass loss rate over the red supergiant phase. The most massive black hole that can be formed from the present models at Z = 0.006 is around 55 M ⊙ . No model in the range of mass considered will enter into the pair-instability supernova regime, while the minimal mass to enter the region of pair pulsation instability is around 60 M ⊙ for the rotating models and 85 M ⊙ for the nonrotating ones. Conclusions. The present models are of particular interest for comparisons with observations in the LMC and also in the outer regions of the Milky Way. We provide public access to numerical tables that can be used for computing interpolated tracks and for population synthesis studies. Stars evolution Stars rotation Stars abundances Dewey 520 26 Département d'astronomie 12 false Astronomy & astrophysics 652 ddc37c9e-348f-48c8-b1da-afe3df079766 Article (Submitted version) Public Article-scientifique-from-unpaywall.pdf 1777421 application/pdf 20b5e246-c081-4ce4-826c-f1dadb8aca10 Article (Published version) Public aa41222-21.pdf 1630527 application/pdf openAccess Faculté des sciences / Département d'astronomie

Title	Published in	Year	Views	Downloads

Very Massive Stars: Near and Far	Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far	2022	9	0
Physics of very massive stars along the cosmic history		2022	425	191
Grids of stellar models with rotation	Astronomy & astrophysics	2021	290	838

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