Grids of stellar models with rotation - I. Models from 0.8 to 120 M⊙ at solar metallicity (Z = 0.014)

By S. Ekström, C. Georgy, P. Eggenberger, G. Meynet, Nami Mowlavi, A. Wyttenbach, A. Granada, T. Decressin, R. Hirschi, U. Frischknecht and 2 more. 2011

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Aims. Many topical astrophysical research areas, such as the properties of planet host stars, the nature of the progenitors of different types of supernovae and gamma ray bursts, and the evolution of galaxies, require complete and homogeneous sets of stellar models at different metallicities in order to be studied during the whole of cosmic history. We present here a first set of models for solar metallicity, where the effects of rotation are accounted for in a homogeneous way. Methods. We computed a grid of 48 different stellar evolutionary tracks, both rotating and non-rotating, at Z = 0.014, spanning a wide mass range from 0.8 to 120 M� . For each of the stellar masses considered, electronic tables provide data for 400 stages along the evolutionary track and at each stage, a set of 43 physical data are given. These grids thus provide an extensive and detailed data basis for comparisons with the observations. The rotating models start on the zero-age main sequence (ZAMS) with a rotation rate υini/υcrit = 0.4. The evolution is computed until the end of the central carbon-burning phase, the early asymptotic giant branch (AGB) phase, or the core helium-flash for, respectively, the massive, intermediate, and both low and very low mass stars. The initial abundances are those deduced by Asplund and collaborators, which best fit the observed abundances of massive stars in the solar neighbourhood. We update both the opacities and nuclear reaction rates, and introduce new prescriptions for the mass-loss rates as stars approach the Eddington and/or the critical velocity. We account for both atomic diffusion and magnetic braking in our low-mass star models. Results. The present rotating models provide a good description of the average evolution of non-interacting stars. In particular, they reproduce the observed main-sequence width, the positions of the red giant and supergiant stars in the Hertzsprung-Russell (HR) diagram, the observed surface compositions and rotational velocities. Very interestingly, the enhancement of the mass loss during

Subfields: Astronomy and Astrophysics

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Citations in the corpus

The VLT-FLAMES Tarantula Survey XXVII. Physical parameters of B-type main-sequence binary systems in the Tarantula nebula (2017, positive): “These developments have allowed the generation of extensive grids of evolutionary models (see, for example, Brott et al. 2011a; Ekström et al. 2012; Georgy et al. 2013), which have been used to synthesize stellar populations for comparison with the results from large-scale surveys (Brott et al.…”
Evolution and fate of very massive stars (2013, methodology): “The full list of updated rates and a short description of the effects on stellar evolution are presented in Ekström et al. (2012).”
A PANCHROMATIC VIEW OF THE RESTLESS SN 2009ip REVEALS THE EXPLOSIVE EJECTION OF A MASSIVE STAR ENVELOPE (2013, methodology): “PPI leads to partial unbinding of the star, with a sequence of eruptions 64 This is the velocity required to reach Rbo after∼ 50 days since the 2012a explosion.”
The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, background): “However, other recent models have considered alternative evolutionary scenarios whereby LGRB progenitors can lose a great deal of mass before exploding, but still retain enough angular momentum to power a GRB [313, 314, 315].”
Presupernova Evolution and Explosive Nucleosynthesis of Rotating Massive Stars in the Metallicity Range −3 ≤ [Fe/H] ≤ 0 (2018, background): “…& Maeder 2003; Heger et al. 2005; Meynet & Maeder 2005; Brott et al. 2011; Limongi & Chieffi 2012; Chieffi & Limongi 2013; Maeder & Meynet 2012; Ekström et al. 2012), a homogeneous and extended set (in mass, metallicity, initial rotation velocity, and number of nuclear species followed) is…”
Multiplicity of Galactic Cepheids from long-baseline interferometry – III. Sub-percent limits on the relative brightness of a close companion of δ Cephei (2016, methodology): “We retrieved Geneva stellar isochrones (Ekström et al. 2012) for ages t = 95 − 125 Myr, a solar metallicity Z = 0.014 and a initial rotation rate of Ω/Ωcrit = 0.568.”
Merging binary black holes formed through chemically homogeneous evolution in short-period stellar binaries (2015, background): “Rotation has become a standard ingredient in various evolutionary codes (e.g., Maeder & Meynet 2000; Heger et al. 2000; Potter et al. 2012; Paxton et al. 2013) and extensive model grids of single stars are now becoming available (e.g., Brott et al. 2011a; Ekström et al. 2012; Köhler et al. 2015).”
THE EFFECTS OF STELLAR ROTATION. II. A COMPREHENSIVE SET OF STARBURST99 MODELS (2014, background): “Since then, the Geneva group has generated complete sets of evolutionary tracks for solar and subsolar chemical composition in a format compatible for population synthesis (Ekstrom et al. 2012 (E12); Georgy et al. 2013 (G13)).”
Massive double compact object mergers: gravitational wave sources and r-process element production sites (2013, background): “Note that other groups that study massive single star evolution who used De Jager et al. rates for RSGs have recently adapted their evolutionary code and also use larger RSG rates (Georgy, 2012; Georgy et al., 2012; Ekstrom et al., 2012).”
Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014 (2012, result): “In the present work, we aim to make progress towards providing answers to the above questions, analysing the results we have obtained in our most recent solar-metallicity grid of stellar models (Ekström et al. 2012, hereafter Paper I) .”
STELLAR POPULATIONS IN THE CENTRAL 0.5 pc OF THE GALAXY. II. THE INITIAL MASS FUNCTION (2013, background): “…photometry differs by .2% in the K-band, which is less than our photometric precision, so no interpolation between the different atmosphere mod- 7 Ekström et al. (2012) contains an updated grid of Geneva models with rotation extending down to lower masses and with rotation speeds other than…”
The star formation history and accretion-disc fraction among the K-type members of the Scorpius–Centaurus OB association (2016, methodology): “Our stellar parameters for the main-sequence turn-off in ScoCen are listed in Table 10, along with an individual age estimate of each object from a comparison the rotating tracks of Ekström et al. (2012), rotating at veq = 0.4vcrit , with the H-R diagram position of the stars.”
Forming short-period Wolf–Rayet X-ray binaries and double black holes through stable mass transfer (2017, methodology): “To calculate the outcome of CE evolution for stars in the mass range 10 to 85 M we used the rotating evolutionary models for solar metallicity of Ekström et al. (2012).”
Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, background): “…incorporate important advances achieved over the past decade in the theories of stellar interiors (e.g., Eldridge et al. 2008; Bressan et al. 2012; Ekström et al. 2012; Georgy et al. 2013; Chen et al. 2015) and atmospheres (e.g., Hauschildt & Baron 1999; Hillier & Miller 1999; Pauldrach et al.…”