How Massive Single Stars End Their Life

By Alexander Heger, Chris L. Fryer, Stan Woosley, N. Langer, D. Hartmann. 2002

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How massive stars die—what sort of explosion and remnant each produces—depends chiefly on the masses of their helium cores and hydrogen envelopes at death. For single stars, stellar winds are the only means of mass loss, and these are a function of the metallicity of the star. We discuss how metallicity, and a simplified prescription for its effect on mass loss, affects the evolution and final fate of massive stars. We map, as a function of mass and metallicity, where black holes and neutron stars are likely to form and where different types of supernovae are produced. Integrating over an initial mass function, we derive the relative populations as a function of metallicity. Provided that single stars rotate rapidly enough at death, we speculate on stellar populations that might produce gamma-ray bursts and jet-driven supernovae.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7474e4a538b0cbe21e9fdc280a27c88197f17458

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Citations in the corpus

THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “…explosions are not confined to a well-defined range of initial progenitor masses as is usually assumed (e.g. Fryer & Kalogera 2001; Woosley et al. 2002; Heger et al. 2003), but are instead interwoven between the successful ones, as was found also by O’Connor & Ott (2011) and Ugliano et al. (2012).”
The physics of star formation (2003, background): “Metal-poor stars with masses between 140 and 260 M⊙ are predicted to explode completely as very energetic supernovae at the end of their lifetimes, while stars more massive than 260 M⊙ are predicted to collapse completely to black holes (Heger et al 2003).”
Resolving the Formation of Protogalaxies. III. Feedback from the First Stars (2007, background): “Outside of the pair-instability mass range, Pop III stars die by directly collapsing into a BH (Heger et al. 2003), possibly providing the seeds of high-redshift quasars in galaxies that are associated with the rarest density fluctuations (e.g. Madau & Rees 2001; Volonteri et al. 2005; Trenti &…”
The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, background): “To date, the best theoretical stellar models find it hard to produce enough angular momentum in the core at the time of collapse to make a centrifugally supported disk, though some progress has been made [382, 383, 468].”
Dust formation history of galaxies: A critical role of metallicity* for the dust mass growth by accreting materials in the interstellar medium (2012, methodology): “Also, we assume that all stars with initial massesm > 40 M⊙ evolve to black holes without SN explosions (Heger et al., 2003).”
Two populations of LIGO-Virgo black holes (2020, background): “These stars produce the so-called pulsational PISN (PPISN) [26, 104, 105], where the star after several violent pulsational mass loss events leaves behind remnant BH.”
Massive black hole binaries from runaway collisions: the impact of metallicity (2016, background): “At the end, the merger product may explode as a supernova (SN, Portegies Zwart & van den Heuvel 2007; Pan et al. 2012; van den Heuvel & Portegies Zwart 2013), or it may preserve enough mass to collapse to a BH directly (Fryer 1999; Heger et al. 2003; Fryer et al. 2012; Spera et al. 2015).”
Merging black hole binaries with the SEVN code (2018, background): “…supernovae (SNe) is far from optimal (see Foglizzo et al. 2015 for a recent review), several studies (Fryer 1999; Fryer, Woosley & Heger 2001; Heger et al. 2003; O’Connor & Ott 2011; Fryer et al. 2012; Ugliano et al. 2012; Ertl et al. 2016) suggest that if the mass and/or the compactness of…”
The birth of a galaxy – II. The role of radiation pressure (2012, background): “They die as Type II SNe if 11 6 M⋆/M⊙ 6 40 M⊙ (Woosley & Weaver 1995; Nomoto et al. 2006) and as PISNe if they are in the mass range 140–260 M⊙ (Heger et al. 2003), where M⋆ is the stellar mass.”
THE BIRTH OF A GALAXY: PRIMORDIAL METAL ENRICHMENT AND STELLAR POPULATIONS (2010, positive): “They die as Type II SNe if 11 ≤ M⋆/M⊙ ≤ 40 M⊙ (Woosley & Weaver 1995) and as PISNe if they are in the mass range 140–260M⊙ (Heger et al. 2003), where M⋆ is the stellar mass.”
Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014 (2012, background): “…Georgy et al. (2009), where no distinction was considered between the various subtypes of type II SNe, we add in this work the same criterion as in Heger et al. (2003) to distinguish between the type II-P SNe, and the type II-L or II-b SNe (owing to the weak statistics of these events, there is…”
Formation of z~6 Quasars from Hierarchical Galaxy Mergers (2006, background): “Recent theory of Population III star formation predicts a mass range of 30Y500M , but there are two regimes where an SMBH could form, either 100M or 260M (Heger et al. 2003; for a recent discussion see also Yoshida et al. 2006).”
Massive stars exploding in a He-rich circumstellar medium. I. Type Ibn (SN 2006jc-like) events (2008, background): “However current stellar evolutionary theory would not predictthat such η-Car type objects would undergo core-collapse so close (2 years) to the LBV stage (Heger et al. 2003; Eldridge & Vink 2006).”
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).”