Short Gamma-Ray Bursts from the Merger of Two Black Holes

TL;DR

This paper proposes a new model where two high-mass, low-metallicity stars can produce a short gamma-ray burst from black hole mergers without requiring a neutron star, challenging previous assumptions.

Contribution

It introduces a novel scenario where black hole mergers can generate short GRBs through a process involving stellar evolution and disk re-ignition, without neutron stars.

Findings

A new stellar evolution pathway can produce short GRBs from black hole mergers.

The model explains the Fermi satellite's detection of a GRB with GW150914.

Long-lived disks can be re-ignited during pre-merger, powering short GRBs.

Abstract

Short Gamma-Ray Bursts (GRBs) are explosions of cosmic origin believed to be associated with the merger of two compact objects, either two neutron stars, or a neutron star and a black hole. The presence of at least one neutron star has long been thought to be an essential element of the model: its tidal disruption provides the needed baryonic material whose rapid accretion onto the post-merger black hole powers the burst. The recent tentative detection by the Fermi satellite of a short GRB in association with the gravitational wave signal GW150914 produced by the merger of two black holes has challenged this standard paradigm. Here we show that the evolution of two high-mass, low-metallicity stars with main sequence rotational speeds a few tens of percent of the critical speed eventually undergoing a weak supernova explosion {\em can} produce a short gamma-ray burst. The outer layers of the envelope of the last exploding star remain bound and circularize at large radii. With time, the disk cools and becomes neutral, suppressing the magneto-rotational instability, and hence the viscosity. The disk remains 'long-lived dead' until tidal torques and shocks during the pre-merger phase heat it up and re-ignite accretion, rapidly consuming the disk and powering the short gamma-ray burst.