Swift 1644+57: The Longest Gamma-ray Burst?

TL;DR

This paper explores whether the unusual long-lasting gamma-ray and x-ray transient Sw 1644+57 is a long-duration gamma-ray burst or an outburst from a supermassive black hole, analyzing possible progenitors and powering mechanisms.

Contribution

It proposes and discusses the possibility that Sw 1644+57 is a very long-duration, low-power GRB-like transient from core-collapse events, connecting it to magnetar spindown and faint supernovae.

Findings

Sw 1644+57's properties are consistent with very long-duration, low-power GRB models.

Both neutron star and black hole models can produce jets capable of powering the observed emission.

The event may be linked to the collapse of a red supergiant in a failed supernova scenario.

Abstract

Swift recently discovered an unusual gamma-ray and x-ray transient (Sw 1644+57) that was initially identified as a long-duration gamma-ray burst (GRB). However, the ~ 10 keV x-ray emission has persisted for over a month with a luminosity comparable to its peak value. The astrometric coincidence of the source with the center of its host galaxy, together with other considerations, motivated the interpretation that Sw 1644+57 was produced by an outburst from a 10^{6-7} M_sun black hole at the center of the galaxy. Here we consider the alternate possibility that Sw 1644+57 is indeed a long-duration GRB, albeit a particularly long one. We discuss the general properties of very long-duration, low-power GRB-like transients associated with the core-collapse of a massive star. Both neutron star (magnetar) spindown and black hole accretion can power such events. The requirements for producing low-power, very long-duration GRBs by magnetar spindown are similar to those for powering extremely luminous supernovae by magnetar spindown, suggesting a possible connection between these two unusual types of transients. Alternatively, Sw 1644+57 be associated with the faintest core-collapse explosions: the collapse of a rotating red supergiant in a nominally failed supernova can power accretion onto a solar-mass black hole for up to ~ 100 days; the jet produced by black hole accretion inevitably unbinds the outer envelope of the progenitor, leading to a weak ~ 10^{49} erg explosion. In both neutron star and black hole models, a jet can burrow through the host star in a few days, with a kinetic luminosity ~ 10^{45-46} ergs/s, sufficient to power the observed emission of Sw 1644+57.