Spectral Properties of X-Ray Flares in Gamma-Ray Bursts

Abstract We conducted a systematic spectral analysis of the X-ray flares of gamma-ray bursts (GRBs) observed by Swift/X-ray Telescope from 2005 April to 2015 March. The sample includes 521 flares from 206 GRBs. The GRBs cover the three subtypes: X-ray flashes (XRFs), X-ray-rich GRBs (XRRs), and classical GRBs (C-GRBs). We used a simple power-law model to fit the spectra during the flares, as well as to fit the preflare and postflare afterglow emissions, and obtained the parameters such as photon index and intrinsic hydrogen column density ( N H ). By comparing the spectral characteristics of flares, prompt emission, and afterglow emission, and analyzing the temporal evolution of the X-ray flare spectra, we obtained the following main conclusions. (1) The spectrum during the flare phase is significantly harder than that of the preflare and postflare phases, while there is no obvious difference in the spectrum between the preflare and postflare phases. (2) The intrinsic N H shows no significant change between the preflare and flare phases, but significantly decreases after the flare. (3) The overall X-ray flare spectra are softer than those of the prompt emission. (4) For GRBs with multiple flares, the photon index softens with increasing flare peak time. (5) The X-ray flare spectra in XRFs are softer than those in C-GRBs. These results support the origin of X-ray flares being from the internal shock radiation driven by the late activity of the GRB central engine.