Progenitors of Long-Duration Gamma-ray Bursts

TL;DR

This paper reviews models of massive star progenitors for long-duration gamma-ray bursts, discusses observational evidence linking LGRBs with supernovae, and evaluates single versus binary star scenarios, highlighting the potential of chemically homogeneous evolution.

Contribution

It introduces detailed stellar models across a range of masses and rotation rates, and analyzes their implications for LGRB progenitors and observed rates, including the role of CHE.

Findings

Chemically homogeneous evolution may be the main pathway for LGRB production.

Binary channels are less likely to produce LGRBs matching observed rates.

Progenitor metallicity and rotation influence LGRB likelihood and characteristics.

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 $10\text{--}150 \, \mathrm{M}_\odot$ with $\Delta \mathrm{M}=10 \, \mathrm{M}_\odot$ and rotation rate $v/v_{\rm{crit}}=0$ to $0.6$ with a velocity resolution $\Delta v/v_{\rm{crit}} =0.1$. 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.