Rotating massive main-sequence stars - I. Grids of evolutionary models and isochrones

By I. Brott, Selma de Mink, Matteo Cantiello, N. Langer, A. D. Koter, C. Evans, I. Hunter, C. Trundle, J. Vink. 2011

245 citations recorded by the source corpus.

We present a dense grid of evolutionary tracks and isochrones of rotating massive main-sequence stars. We provide three grids with different initial compositions tailored to compare with early OB stars in the Small and Large Magellanic Clouds and in the Galaxy. Each grid covers masses ranging from 5 to 60 M and initial rotation rates between 0 and about 600 km s−1. To calibrate our models we used the results of the VLT-FLAMES Survey of Massive Stars. We determine the amount of convective overshooting by using the observed drop in rotation rates for stars with surface gravities logg <3.2 to determine the width of the main sequence. We calibrate the efficiency of rotationally induced mixing using the nitrogen abundance determinations for B stars in the Large Magellanic cloud. We describe and provide evolutionary tracks and the evolution of the central and surface abundances. In particular, we discuss the occurrence of quasi-chemically homogeneous evolution, i.e. the severe effects of efficient mixing of the stellar interior found for the most massive fast rotators. We provide a detailed set of isochrones for rotating stars. Rotation as an initial parameter leads to a degeneracy between the age and the mass of massive main sequence stars if determined from its observed location in the Hertzsprung-Russell diagram. We show that the consideration of surface abundances can resolve this degeneracy.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/0f6656da161f276a21f32de5e6757842769798ef

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Citations in the corpus

THE ROTATION RATES OF MASSIVE STARS: THE ROLE OF BINARY INTERACTION THROUGH TIDES, MASS TRANSFER, AND MERGERS (2012, methodology): “The internal rotational profile is approximated assuming rigid rotation, which is a reasonable approximation for main-sequence stars (e.g., Brott et al. 2011a).”
Stellar winds on the main-sequence - II. The evolution of rotation and winds (2015, methodology): “For the stellar evolution calculations, we use the 1D hydrodynamic stellar evolution code described in Heger et al. (2000), Brott et al. (2011a), and Brott et al. (2011b).”
Merging binary black holes formed through chemically homogeneous evolution in short-period stellar binaries (2015, methodology): “Brott et al. (2011a) and Köhler et al. (2015) further explored a larger range of masses and higher metallicities using models where the efficiency of rotational mixing is calibrated against the observed nitrogen abundances of early B type stars in the Large Magellanic Cloud.”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, methodology): “…treatment is often calibrated to fit the observed MSTO of stellar clusters and associations, and is a commonly adopted scheme in many stellar evolution codes (e.g., Demarque et al. 2004; Pietrinferni et al. 2004; Dotter et al. 2008; Brott et al. 2011a; Bressan et al. 2012; Ekström et al. 2012).”
Wind modelling of very massive stars up to 300 solar masses (2011, methodology): “These high Ω values of the order of 0.85 seem to be rather high when we consider recent stellar evolution models (Brott et al. 2011; Friedrich et al. in prep.)”
The VLT-FLAMES Tarantula Survey XXVII. Physical parameters of B-type main-sequence binary systems in the Tarantula nebula (2017, unknown): “Also shown are the evolutionary tracks and isochrones of Brott et al. (2011a) for e ﬀ ectively zero initial rotational velocity.”
THE ORIGIN AND OPTICAL DEPTH OF IONIZING RADIATION IN THE “GREEN PEA” GALAXIES (2013, background): “The highest mass stars are the most likely to evolve homogeneously and reach such high temperatures (e.g., Brott et al. 2011a).”
The chemically homogeneous evolutionary channel for binary black hole mergers: rates and properties of gravitational-wave events detectable by advanced LIGO (2016, background): “Originally these processes have been considered in the case of rotating single stars and have been proposed as an explanation for surface abundance anomalies such as nitrogen enhancements (e.g., Maeder & Meynet 2000, see however Brott et al. 2011).”
Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, methodology): “In the present case, a better calibration is adopted: the models fit the main trend of N abundance versus initial rotational velocity observed in a sample of stars taken from the FLAMES survey of the LMC (the so called Hunter diagram, Hunter et al. 2009), as originally done by Brott et al. (2011).”
THE INCIDENCE OF STELLAR MERGERS AND MASS GAINERS AMONG MASSIVE STARS (2013, methodology): “A more direct motivation is the need to test state-ofthe-art stellar evolution models, which contain uncertain effects of convection, rotation and magnetic fields (e.g. Brott et al. 2011a; Ekström et al. 2012; Potter et al. 2012).”
INTERNAL GRAVITY WAVES IN MASSIVE STARS: ANGULAR MOMENTUM TRANSPORT (2013, background): “These stars contradict models which predict that rotational velocity should be correlated with surface nitrogen enhancement (Brott et al. 2011).”