Abstract
We review the current scenario of long-duration Gamma-ray burst (LGRB) progenitors, and in addition, present models of massive stars for a mass range of 10–150M⊙ with ΔM=10M⊙ and rotation rate v/vcrit=0 to 0.6 with a velocity resolution Δv/vcrit=0.1. We further discuss possible metallicity and rotation rate distribution from our models that might be preferable for the creation of successful LGRB candidates given the observed LGRB rates and their metallicity evolution. In the current understanding, LGRBs are associated with Type-Ic supernovae (SNe). To establish LGRB-SN correlation, we discuss three observational paths: (i) space-time coincidence, (ii) evidence from photometric light curves of LGRB afterglows and SN Type-Ic, (iii) spectroscopic study of both LGRB afterglow and SN. Superluminous SNe are also believed to have the same origin as LGRBs. Therefore, we discuss constraints on the progenitor parameters that can possibly dissociate these two events from a theoretical perspective. We further discuss the scenario of single star versus binary star as a more probable pathway to create LGRBs. Given the limited parameter space in the mass, mass ratio and separation between the two components in a binary, binary channel is less likely to create LGRBs to match the observed LGRB rate. Despite effectively-single massive stars are fewer in number compared to interacting binaries, their chemically homogeneous evolution (CHE) might be the major channel for LGRB production.
Highlights
Gamma-ray bursts (GRBs) are intense flashes of high energy electromagnetic radiation of ∼a few 100 keV with a very brief duration of 1 s to a few minutes reaching Earth isotropically from unpredictable directions
This paper aims to review the possible progenitors of long-duration Gamma-ray burst (LGRB), find the connection between CCSNe and GRB, and dissociate progenitors of LGRB and SLSN based on several theoretical constraints on the pre-SN cores
We present a set of models of massive stars for varying mass, rotation rate and metallicity to narrow down a range of values that are favoured by the observed LGRB rate and its metallicity evolution
Summary
Gamma-ray bursts (GRBs) are intense flashes of high energy electromagnetic radiation of ∼a few 100 keV with a very brief duration of 1 s to a few minutes reaching Earth isotropically from unpredictable directions. One can study spectroscopy to establish the SN-GRB connection Another class of SNe, Type I superluminous supernovae ( SLSNe), is believed to have a similar origin as LGRBs. SLSNe are characterized by luminosities. 10–100 times larger than “typical” SNe [8,9,10], and their 56 Ni mass of ∼20–30 M is much higher compared to 1 M for “typical” SNe ([11] and references therein) Their spectra show the absence of H and He, same as Type-Ic SN, and they are bare carbon and oxygen cores [12]. Several recent theoretical models invoke a few diagnostic parameters of the progenitors at the pre-SN or pre-collapse phase that determine the final fates [14,15,16,17] One such diagnostic parameter is the “so-called” core compactness parameter, ξ M [14]. This paper is organized as follows: in Section 2, we discuss the existing observations that associate SNe with LGRBs; in Section 3, we present the leading models for the progenitors of SLSNe and LGRBs; in Section 4, we illustrate whether single or binary stars are more suitable candidates for LGRB progenitors; in Section 5, we describe the properties of WR stars that are required to form LGRB progenitors, and in Section 6, we summarise the salient points of this review article and pose the open questions that will be the focus of research for LGRB astrophysics in the coming years
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