Presupernova Evolution of Massive Single and Binary Stars

By N. Langer. 2012

633 citations recorded by the source corpus.

Understanding massive stars is essential for a variety of branches of astronomy including galaxy and star cluster evolution, nucleosynthesis and supernovae, pulsars, and black holes. It has become evident that massive star evolution is very diverse, being sensitive to metallicity, binarity, rotation, and possibly magnetic fields. Although the problem to obtain a good statistical observational database is alleviated by current large spectroscopic surveys, it remains a challenge to model these diverse paths of massive stars toward their violent end stage. I show that the main sequence stage offers the best opportunity to gauge the relevance of the various possible evolutionary scenarios. This also allows sketching the post-main-sequence evolution of massive stars, for which observations of Wolf-Rayet stars give essential clues. Recent supernova discoveries owing to the current boost in transient searches allow tentative mappings of progenitor models with supernova types, including pair-instability supernova...

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/9aed4efd12af0a0c04e8408b36f3acc83516eee3

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Citations in the corpus

Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “The core rotational angular momentum before the supernova can be changed from the birth spin of the progenitor by several processes(Langer 2012; de Mink et al. 2013; Amaro-Seoane & Chen 2016).”
The VLT-FLAMES Tarantula Survey XXVII. Physical parameters of B-type main-sequence binary systems in the Tarantula nebula (2017, neutral): “With the development of both observational and theoretical techniques is has been possible to move from the pioneer-⋆ for example, Maeder 2009; Langer 2012).”
THE EFFECTS OF STELLAR ROTATION. II. A COMPREHENSIVE SET OF STARBURST99 MODELS (2014, background): “Recent work has suggested that at least 50% of all massive stars are in binaries and that close to 70% of (A color version of this figure is available in the online journal.) massive binaries are interacting in the course of their evolution (Langer 2012; Sana et al. 2012, 2013).”
Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars (2015, background): “(see Langer 2012, for a recent theoretical overview).”
Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “The donor will likely develop into a WR star when it loses more mass to the companion in what Langer (2012) calls Case AB mass transfer.”
Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results (2017, background): “The underlying stellar evolution models are also undergoing an unprecedented increase in accuracy (see e.g. Langer 2012).”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): BINARIES, PULSATIONS, AND EXPLOSIONS (2015, background): “There are many ways M & 8 M stars can end their lives 3 (e.g., Woosley et al. 2002; Smartt 2009; Meynet et al. 2010; Langer 2012; Nomoto et al. 2013; Smith 2014).”
THE ROTATION RATES OF MASSIVE STARS: THE ROLE OF BINARY INTERACTION THROUGH TIDES, MASS TRANSFER, AND MERGERS (2012, background): “Detailed models show that mass transfer in a binary results in surface nitrogen enrichment that covers the observed range (Wellstein et al. 2001; Langer 2012).”
Formation of Double Neutron Star Systems (2017, background): “2006; Mokiem et al. 2007; Markova & Puls 2008; Langer 2012; Šurlan et al. 2013; Chaty 2013; Falanga et al. 2015).”
Super and massive AGB stars - IV. Final fates - Initial to final mass relation (2014, background): “…solar metallicity (Z=0.02) case was presented in Poelarends et al. (2008) whilst an overview for their entire metallicity range provided in fig.12 in Langer (2012) 11 There is a a typographically error in Siess (2007) pg.905, where the Ṁenv should be 5×10−5 M⊙ yr−1 instead of 5×10−4 M⊙…”
Progenitors of gravitational wave mergers: binary evolution with the stellar grid-based code ComBinE (2018, background): “The metallicity may also have an important effect on the evolution of a star (Langer 2012).”
The IACOB project - I. Rotational velocities in northern Galactic O- and early B-type stars revisited. The impact of other sources of line-broadening (2013, background): “…15 years since Maeder & Meynet (2000) highlighted thatrotation is indispensable for a proper modeling of the evolution for the upper Main Sequence stars in their review about the evolution of rotating massive stars (see also the more recent review by Langer, 2012 and references in both documents).”
Massive double compact object mergers: gravitational wave sources and r-process element production sites (2013, background): “This means that during the RLOF in case A binaries the gasstream from the mass loser will hit directly the mass gainer (instead of first forming a Keplerian disk which is the case in case Br binaries) and this favors conservative mass transfer (for a review see Langer, 2012).”
A new route towards merging massive black holes (2016, background): “The BH progenitors in the systems above the gap also become pair unstable, but the explosive burning cannot reverse the collapse, which leads straight to the formation of a black hole (Heger & Woosley 2002; Langer 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).”
Fundamental properties of core-collapse Supernova and GRB progenitors: predicting the look of massive stars before death (2013, background): “Mass loss and angular momentum evolution play a key role in determining the properties of massive stars across their evolution and the properties of the SN progenitor and the ensuing explosion (for recent reviews see Maeder & Meynet 2012; Langer 2012).”
Ultra-stripped supernovae: progenitors and fate (2015, background): “The main effects, besides from mass loss/gain, are changes in the stellar rotation rate, the nuclear burning scheme and the wind mass-lossrate (de Mink 2010; Langer 2012).”