The Supernova–Gamma-Ray Burst Connection

Abstract

Observations show that at least some gamma-ray bursts (GRBs) happen simultaneously with core-collapse supernovae (SNe), thus linking by a common thread nature's two grandest explosions. We review here the growing evidence for and theoretical implications of this association, and conclude that most long-duration soft-spectrum GRBs are accompanied by massive stellar explosions (GRB-SNe). The kinetic energy and luminosity of well-studied GRB-SNe appear to be greater than those of ordinary SNe, but evidence exists, even in a limited sample, for considerable diversity. The existing sample also suggests that most of the energy in the explosion is contained in nonrelativistic ejecta (producing the supernova) rather than in the relativistic jets responsible for making the burst and its afterglow.

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

“…Long-duration γ-ray bursts (GRBs) have been firmly established to originate from the catastrophic death of massive stars (e.g., Woosley & Bloom 2006). The large luminosities of GRB afterglows make these energetic events premier probes of the high-redshift universe, ranging from the parsec-scale environments of the progenitors to the properties of the intergalactic medium (Totani et al 2006;Inoue et al 2007;Tanvir et al 2009;Wang et al 2012;Chornock et al 2013Chornock et al , 2014.…”

Models for GRBs and diverse transients

“…In particular, they might have lower average energy and be more affected by a higher-density circumstellar environment. GRBs are frequently, perhaps universally accompanied by bright Type Ic-BL supernovae (Woosley & Bloom 2006). Indeed, it is difficult to imagine the production of a relativistic jet in a massive star by any means that does not require the star's death and at least partial disruption, and the evidence linking most long-soft GRBs to massive stars is strong.…”

“…For greater detail see Zhang & Woosley (in preparation). provided something (neutrinos?) can hold up the accreting star while the 'protoneutron star' experiences several seconds of Kelvin-Helmholtz evolution and shrinks to its final radius, rotation rate and magnetic field strength Woosley & Bloom 2006). To explain GRBs in the highest metallicity regions (i.e.…”

Pulsar kicks andγ-ray burst

“…The discovery of 4 clear associations (and many SN bumps in the late optical afterglow light curves) between long, soft GRBs and Type II/Ibc SNe (see, e.g., the review by Woosley & Bloom 2006) results in finding common explosive processes for SNe and GRBs to form rapidly spinning black holes (Woosley 1993), neutron stars (Kluźniak & Ruderman 1998), or even quark stars (Dai & Lu 1998). It is worth noting that GRB as a signature of phase transition to quark-gluon plasma (Xu et al 1999;Wang et al 2000;Yasutake et al 2005;Paczyński & Haensel 2005;Drago et al 2007;Haensel & Zdunik 2007) has also wide implications for the study of elementary interactions between quarks.…”