Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014

By C. Georgy, S. Ekström, G. Meynet, Philip Massey, Emily M. Levesque, R. Hirschi, P. Eggenberger, Andre Maeder. 2012

214 citations recorded by the source corpus.

Context. In recent years, many very interesting observations have appeared concerning the positions of Wolf-Rayet (WR) stars in the Hertzsprung-Russell diagram (HRD), the number ratios of WR stars, the nature of Type Ibc supernova (SN) progenitors, long and soft gamma ray bursts (LGRB), and the frequency of these various types of explosive events. These observations represent key constraints on massive star evolution. Aims. We study, in the framework of the single-star evolutionary scenario, how rotation modifies the evolution of a given initial mass star towards the WR phase and how it impacts the rates of Type Ibc SNe. We also discuss the initial conditions required to obtain collapsars and LGRB. Methods. We used a recent grid of stellar models computed with and without rotation to make predictions concerning the WR populations and the frequency of different types of core-collapse SNe. Current rotating models were checked to provide good fits to the following features: solar luminosity and radius at the solar age, main-sequence width, red-giant and red-supergiant (RSG) positions in the HRD, surface abundances, and rotational velocities. Results. Rotating stellar models predict that about half of the observed WR stars and at least half of the Type Ibc SNe may be produced through the single-star evolution channel. Rotation increases the duration of the WNL and WNC phases, while reducing those of the WNE and WC phases, as was already shown in previous works. Rotation increases the frequency of Type Ic SNe. The upper –

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/6d4cb370150d7d91c50d1e7043d407e73e77d1da

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Citations in the corpus

• Luminous blue variables are antisocial: their isolation implies that they are kicked mass gainers in binary evolution (2014, background): “With or without including rapid rotation, single-star models typically expect WC stars to arise from the most massive stars and not an intermediate mass range (e.g., Georgy et al. 2012; Heger et al. 2003).”
• MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, methodology): “The red circles are observations from Neugent & Massey (2011) and Neugent et al. (2012), and the blue diamond point is the observed ratio computed by Georgy et al. (2012), estimated in the 3 kpc radius volume around the solar neighborhood (see their Section 4.4 for references therein).”
• Fundamental properties of core-collapse Supernova and GRB progenitors: predicting the look of massive stars before death (2013, methodology): “We assume, as in Georgy et al. (2012), a Salpeter-type initial mass function, that the lower and upper initial mass limit for core-collapse SNe are 8 and 120 M , respectively, that SNe occur even when black holes are formed, and that all SNe are observable (see also Heger et al. 2003).”
• On the nature of supernovae Ib and Ic (2012, background): “…a 25 M star in a binary system at solar metallicity, with, at the time of explosion, a mass of 4.41 7 In future work, we will investigate a broader range of progenitors, including single rotating and non-rotating WR stars (Georgy et al. 2012), and wider interacting binaries (Claeys et al. 2011).”
• A PANCHROMATIC VIEW OF THE RESTLESS SN 2009ip REVEALS THE EXPLOSIVE EJECTION OF A MASSIVE STAR ENVELOPE (2013, background): “Standard stellar evolutionary models predict massive stars with M & 40M to spend half a Myr in the Wolf-Rayet (WR) phase before exploding as supernovae (SNe, e.g. Georgy et al. 2012 and references therein).”
• 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].”
• The spin of the second-born black hole in coalescing binary black holes (2018, background): “In cases angular momentum is transported mainly by meridional currents, the coupling is less efficient (e.g., Georgy et al. 2012) allowing the core to retain more angular momentum.”
• Physical Processes in the Interstellar Medium (2014, background): “…also note that stellar rotation can dramatically change the derived stellar mass loss rates and the energy and momentum inserted by line-driven winds (for recent reviews, see Meynet 2009 or Maeder & Meynet 2012, or for a grid of evolutionary tracks, see Ekström et al. 2012 and Georgy et al. 2012).”
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “Standard single-star models predict MWR ≃ 35M⊙ at Z⊙ (Georgy et al. 2012, Heger et al. 2003), in- 26 Smith creasing to about 45 and 70M⊙ at ZLMC and ZSMC , respectively (Heger et al. 2003).”
• PRE-SUPERNOVA EVOLUTION OF ROTATING SOLAR METALLICITY STARS IN THE MASS RANGE 13–120 M☉ AND THEIR EXPLOSIVE YIELDS (2012, background): “Before closing this section let us note that the limiting masses recently obtained by the Geneva group (Georgy et al. 2012) are in good agreement with the present findings.”
• Evolution and fate of very massive stars (2013, methodology): “…in Crowther et al. (2010) and complements the low- and high-mass stellar grids at solar metallicity (Z = 0.014) calculated by Ekström et al. (2012) and Georgy et al. (2012) as well as their extension to lower metallicities (Eggenberger et al., in preparation; Georgy et al., in preparation).”
• Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, background): “For high-metallicity stars, the effects of rotation on the CO core mass are suppressed due to angular momentum loss through stellar winds (Georgy et al. 2012).”
• 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).”
• The SILCC project - III. Regulation of star formation and outflows by stellar winds and supernovae (2016, background): “…from the tracks by Ekström et al. (2012, for the corresponding scaling relations, see their section 2.6), we estimate terminal velocities (vwind), which are not given in the tracks, according to their evolutionary status (defined from the surface abundances of the models, see Georgy et al. 2012).”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, background): “Moreover, the final fate of a massive star depends chiefly on the relative importance of rotation during its evolution (e.g., Heger et al. 2000; Hirschi et al. 2004; Heger et al. 2005; Yoon et al. 2006; Woosley & Heger 2006; Ekström et al. 2012; Georgy et al. 2012; Langer 2012).”
• THE EFFECTS OF STELLAR ROTATION. II. A COMPREHENSIVE SET OF STARBURST99 MODELS (2014, background): “Georgy et al. (2012) estimated that approximately 40% of all W-R stars form via the binary channel at solar chemical composition.”