Grids of stellar models with rotation

Abstract

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.

Grids of stellar models with rotation VII: Models from 0.8 to 300 M$_\odot$ at super-solar metallicity (Z = 0.020)

“…In this paper, we present a grid of stellar models at super-solar metallicity (Z = 0.020) covering a wide range of initial masses from 0.8 to 300 M . This grid extends the previous grids of Geneva models at solar and sub-solar metallicities (Ekström et al 2012;Eggenberger et al 2021;Georgy et al 2013;Groh et al 2019;Murphy et al 2021) and thus uses the same physical ingredients and metallicity dependencies. A metallicity of Z = 0.020 was chosen to match that of the inner Galactic disk.…”

“…Grids of single star models with and without rotation at Z = 0.014, 0.006, 0.002, 0.0004, 0.0, thus covering a wide range of metallicities from solar to primordial stars via the metallicities of the LMC, SMC and I Zw 18 (Ekström et al 2012;Eggenberger et al 2021;Georgy et al 2013;Groh et al 2019;Murphy et al 2021) have been completed using the Geneva Stellar Evolution Code (GENEC; see Eggenberger et al 2008, for details). This paper extends the GENEVA grids of models to super-solar metallicity.…”

Locating Red Supergiants in the Galaxy NGC 6822

“…We compared our observations with theoretical predictions from two different stellar evolutionary codes: the Geneva evolutionary models (Eggenberger et al 2021), which focus on single-star evolution as well as the Binary Population and Spectral Synthesis (BPASS) models (Eldridge et al 2017;Stanway & Eldridge 2018), which include both single and binary star evolution. For both of these evolutionary codes, we used the LMC metallicity (z = 0.006) models.…”

“…For both of these evolutionary codes, we used the LMC metallicity (z = 0.006) models. (Eggenberger et al 2021). Rotating models are shown in solid lines and non-rotating models are shown in dashed lines.…”

“…Uncertainty values for all points are shown in the upper right corner with further discussion in the text. The tracks displayed represent a stellar mass range of 9 to 25M for z = 0.006(Eggenberger et al 2021). Rotating models are shown in solid lines and non-rotating models are shown in dashed lines.…”