Stellar evolution with rotation XII. Pre-supernova models

By R. Hirschi, G. Meynet, Andre Maeder. 2004

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We describe the latest developments of the Geneva stellar evolution code in order to model the pre-supernova evolution of rotating massive stars. Rotating and non-rotating stellar models at solar metallicity with masses equal to 12, 15, 20, 25, 40 and 60 Mwere computed from the ZAMS until the end of the core silicon burning phase. We took into account meridional circulation, secular shear instabilities, horizontal turbulence and dynamical shear instabilities. We find that dynamical shear instabilities mainly smoothen the sharp angular velocity gradients but do not transport angular momentum or chemical species over long distances. Most of the differences between the pre-supernova structures obtained from rotating and non-rotating stellar models have their origin in the effects of rotation during the core hydrogen and helium burning phases. The advanced stellar evolutionary stages appear too short in time to allow the rotational instabilities considered in this work to have a significant impact during the late stages. In particular, the internal angular momentum does not change significantly during the advanced stages of the evolution. We can therefore have a good estimate of the final angular momentum at the end of the core helium burning phase. The effects of rotation on pre-supernova models are significant between 15 and 30 M� . Indeed, rotation increases the core sizes (and the yields) by a factor ∼1.5. Above 20 M� , rotation may change the radius or colour of the supernova progenitors (blue instead of red supergiant) and the supernova type (IIb or Ib instead of II). Rotation affects the lower mass limits for radiative core carbon burning, for iron core collapse and for black hole formation. For Wolf-Rayet stars (M > 30 M� ), the pre-supernova structures are mostly affected by the intensities of the stellar winds and less by rotational mixing.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/bb86718cba0e065755428b31f457a3d67fe86a5d

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Citations in the corpus

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).”
On the evolution of rapidly rotating massive white dwarfs towards supernovae or collapses (2005, methodology): “Key aspects of massive star deaths – notably the production of millisecond pulsars, hypernovae and gamma-ray bursts – require rapid rotation (e.g., Woosley 1993; Paczyński 1998; Hirschi et al. 2004; Heger et al. 2004; Petrovic et al. 2005b).”
Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars (2015, methodology): “The end points of three sets of models are plotted in Figure 4 showing the initial mass–final luminosity relation for the STARS models (Eldridge & Tout 2004), the rotating Geneva models of Hirschi et al. (2004) and the KEPLER models of Woosley & Heger (2007).”
Stellar evolution with rotation - XIII. Predicted GRB rates at various Z (2005, background): “Since then, several studies have been devoted to finding which stars can lead to GRBs. Heger et al. (2004), Heger et al. (2005), and Hirschi et al. (2004) looked at massive single star at solar metallicity as progenitors.”
Simulations of Magnetically Driven Supernova and Hypernova Explosions in the Context of Rapid Rotation (2007, background): “However, all credible MHD models require rapid rotation, which the current crop of solar metallicity supernova progenitor models do not have (Hirschi et al. 2004, 2005; Heger et al. 2000, 1 Department of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ 85721;…”
Progenitors of Core-Collapse Supernovae (2009, methodology): “Even the addition of rapid rotation (Vrot ∼300km s −1) in the stellar models still results in 8− 22M⊙ stars becoming red supergiants during core He burning and beyond (Hirschi, Meynet, and Maeder 2004) as long as they avoid chemically homogeneous evolution (Yoon and Langer 2005).”
Very low-metallicity massive stars: - Pre-SN evolution models and primary nitrogen production (2006, methodology): “The stellar evolution model used to calculate the stellar models is described in detail in Hirschi et al. (2004).”
Evolution and fate of very massive stars (2013, background): “12 in Hirschi et al. 2004) with a radiative core C burning followed by a large convective C-burning shell, radiative neon burning and convective oxygen and silicon-burning stages.”
A strong case for fast stellar rotation at very low metallicities (2006, result): “…that for metallicities Z < 10−5 the yields of nitrogen were strongly increased in comparison to the ones given in MM02 for massive stars (the adopted yields in the case of this model are shown in 2 For the solar metallicity we are adopting the new calculations presented in Hirschi et al. (2004).”
Discovery of an Extraordinarily Massive Cluster of Red Supergiants (2006, background): “Further, rotation rate and metallicity may be important variables, as they affect wind driven mass-loss (Hirschi et al. 2004).”
Non-standard s process in low metallicity massive rotating stars (2011, background): “Rotation significantly changes the structure and pre-SN evolution of massive stars (Hirschi et al., 2004) and thus also the s-process production.”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “…combined with the non-negligible effects of radiation pressure, can significantly alter their evolution (e.g., Heger et al. 2000; Meynet & Maeder 2000; Hirschi et al. 2004; Woosley & Heger 2006; Yoon et al. 2006; de Mink et al. 2010; Georgy et al. 2012; Langer 2012; Köhler et al. 2015).”
s-process production in rotating massive stars at solar and low metallicities (2015, background): “We therefore know that our models would evolve in a similar way as the one of Hirschi et al. (2004), up to the onset of core collapse.”
The Supernova Gamma-Ray Burst Connection (2006, background): “There is general agreement that the omission of magnetic torques leads to cores that do indeed rotate rapidly enough to make a GRB (Heger et al., 2000; Hirschi et al., 2004).”