Flares In Long And Short Gamma Ray Bursts

TL;DR

This paper demonstrates that the cannonball (CB) model effectively explains the similarities and origins of flares in long and short gamma-ray bursts, linking prompt emission, afterglows, and optical flares through common mechanisms.

Contribution

It shows that the CB model's master formulae can accurately reproduce the lightcurves and spectral evolution of X-ray and optical flares in GRBs and SHBs, unifying their understanding.

Findings

CB model reproduces X-ray flare lightcurves and spectra

Flares originate from mass accretion episodes and CB ejections

Optical flares result from CB collisions with surrounding material

Abstract

The many similarities between the prompt emission pulses in gamma ray bursts (GRBs) and X-ray flares during the fast decay and afterglow phases of GRBs suggest a common origin. In the cannonball (CB) model of GRBs, this common origin is mass accretion episodes of fall-back matter on a newly born compact object. The prompt emission pulses are produced by a bipolar jet of highly relativistic plasmoids (CBs) ejected in the early, major episodes of mass accretion. As the accretion material is consumed, one may expect the engine's activity to weaken. X-ray flares ending the prompt emission and during the afterglow phase are produced in such delayed episodes of mass accretion. The common engine, environment and radiation mechanisms (inverse Compton scattering and synchrotron radiation) produce their observed similarities. Flares in both long GRBs and short hard gamma ray bursts (SHBs) can also be produced by bipolar ejections of CBs following a phase transition in compact objects due to loss of angular momentum and/or cooling. Optical flares, however, are mostly produced in collisions of CBs with massive stellar winds/ejecta or with density bumps along their path. In this paper we show that the master formulae of the CB model of GRBs and SHBs, which reproduce very well their prompt emission pulses and their smooth afterglows, seem to reproduce also very well the lightcurves and spectral evolution of the prominent X-ray and optical flares that are well sampled.