Single star progenitors of long gamma-ray bursts - I. Model grids and redshift dependent GRB rate

By Sung-Chul Yoon, N. Langer, C. Norman. 2006

388 citations recorded by the source corpus.

We present grids of massive star evolution models at four different metallicities (Z=0.004, 0.002, 0.001, 0.00001). The effects of rotation on the stellar structure and the transport of angular momentum and chemical elements through the Spruit-Tayler dynamo and rotationally induced instabilities are considered. After discussing uncertainties involved with the adopted physics, we elaborate the final fate of massive stars as a function of initial mass and spin rate, at each considered metallicity. In particular, we investigate for which initial conditions long gamma-ray bursts (GRBs) are expected to be produced in the frame of the collapsar model. Then, using an empirical spin distribution of young massive metal-poor stars and a specified metallicity-dependent history of star-formation, we compute the expected GRB rate as function of metallicity and redshift based on our stellar evolution models. The GRB production in our models is limited to metallicities of Z âa‰ 0.004, with the consequence that about 50% of all GRBs are predicted to be found at redshifts above z = 4, with most supernovae occurring at redshifts below z≃ 2.2. The average GRB/SN ratio predicted by our model is about 1/200 globally, and 1/1250 at low redshift. Future strategies for testing the considered GRB progenitor scenario are briefly discussed.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/67610d5cd5782d5bf41c2b5b3a5ecdf02b74d3b2

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Citations in the corpus

Binary star progenitors of long gamma-ray bursts (2007, methodology): “In particular, it can not be expected that the metallicity threshold for obtaining a long gamma-ray burst (cf. Yoon et al. 2006) can be significantly increased through the type of binary evolution considered here.”
THE ROTATION RATES OF MASSIVE STARS: THE ROLE OF BINARY INTERACTION THROUGH TIDES, MASS TRANSFER, AND MERGERS (2012, background): “…the large implications of rotational mixing on the evolution of the progenitors of long gamma-ray bursts and pair-instability supernovae (e.g., Yoon et al. 2006; Woosley & Heger 2006; Langer et al. 2007) as well as on the chemical and radiative feedback of massive stars, in particular in the…”
PRE-SUPERNOVA EVOLUTION OF ROTATING SOLAR METALLICITY STARS IN THE MASS RANGE 13–120 M☉ AND THEIR EXPLOSIVE YIELDS (2012, neutral): “…and discussed by Meynet & Maeder (2000, 2003); Hirschi et al. (2004); Meynet & Maeder (2005); Decressin et al. (2007); Ekström et al. (2008); Ekström et al. (2012) and Heger et al. (2000); Heger & Langer (2000); Heger et al. (2005); Yoon & Langer (2005); Yoon et al. (2006); Brott et al. (2011).”
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS (2016, background): “…massive stars, allowing them to output large amounts of ionizing radiation tens of million of years after an initial burst of star formation (e.g., Yoon et al. 2006; Eldridge & Stanway 2009, 2012; Levesque et al. 2012; de Mink et al. 2013; Kewley et al. 2013; Leitherer et al. 2014; Szécsi et al.…”
The VLT-FLAMES survey of massive stars: constraints on stellar evolution from the chemical compositions of rapidly rotating Galactic and Magellanic Cloud B-type stars (2009, methodology): “Briefly, these models have been based on the code of Yoon et al. (2006) and include the effects of rotation (Heger et al. 2000) and angular momentum transport via magnetic torques (Spruit 2002).”
NEUTRINO SIGNATURES AND THE NEUTRINO-DRIVEN WIND IN BINARY NEUTRON STAR MERGERS (2008, background): “Similarly, Dessart et al. (2008) found that in collapsar candidates (Woosley & Heger 2006; Yoon et al. 2006; Meynet & Maeder 21 2007), the large amount of free energy of rotation in their iron core at the time of collapse can lead to a magnetically-driven explosion, associated with very large mass…”
Effects of rotation on the evolution of primordial stars (2008, background): “When the magnetic dynamo mechanism proposed by Spruit (1999, 2002) is taken into account, chemical mixing becomes more efficient and homogeneous evolution can be achieved with smaller initial rotation rates (Yoon & Langer 2005; Yoon et al. 2006; Woosley & Heger 2006).”
THE COMPACTNESS OF PRESUPERNOVA STELLAR CORES (2013, methodology): “In our survey αSC was taken to be 0.1 as a ”midpoint” between these two extremes, which is also well within the range used in literature (e.g. Yoon et al. 2006).”
GRB hosts through cosmic time - VLT/X-Shooter emission-line spectroscopy of 96 γ-ray-burst-selected galaxies at 0.1 (2015, background): “These data supported a strong dependence of GRB formation with metallicity (e.g., Hirschi et al. 2005; Yoon et al. 2006) as would be theoretically expected in the collapsar model (Woosley 1993; MacFadyen & Woosley 1999).”
Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results (2017, methodology): “We assume the star must have an effective initial mass after accretion >20 M for this evolution for occur, based on the work of Yoon et al. (2006).”