X-ray flares in GRBs: general considerations and photospheric origin

TL;DR

This paper discusses the physical constraints of X-ray flares in GRBs, proposing a photospheric origin involving a slower outflow launched with the relativistic jet, challenging existing models.

Contribution

It introduces a simple toy model where X-ray flares originate from a modest Lorentz factor outflow launched with the jet, explaining observational features.

Findings

Flare emission region size should be less than 3×10^{14} cm.

Flares are inconsistent with late magnetar spin-down activity.

A slower outflow can produce observable X-ray flares at the photosphere.

Abstract

Observations of X-ray flares from Gamma Ray Bursts (GRBs) imply strong constraints on possible physical models. We provide a general discussion of these. In particular, we show that in order to account for the relatively flat and weak optical flux during the X-ray flares, the size of the emitting region should be $\lesssim 3\times 10^{14}$cm. The bolometric luminosity of flares also strongly constrain the energy budget, and are inconsistent with late time activity of a central engine powered by the spin-down of a magnetar. We provide a simple toy model according to which flares are produced by an outflow of modest Lorentz factor (a few tens instead of hundreds) that is launched more or less simultaneously with the highly relativistic jet which produced the prompt gamma-ray emission. The "slower" moving outflow produces the flare as it reaches its photosphere. The existence of such a component would naturally resolve the observational challenges imposed by flares, outlined in this work.