Observations of X-ray Flares from GRBs

Details Observations of X-ray Flares from GRBs Observations of X-ray Flares from GRBs

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1000...91f&link_type=abstract

GAMMA-RAY BURSTS 2007: Proceedings of the Santa Fe Conference. AIP Conference Proceedings, Volume 1000, pp. 91-96 (2008).

Physics

1

Gamma-Ray Sources, Gamma-Ray Bursts, X-Ray, Distances, Redshifts, Radial Velocities, Spatial Distribution Of Galaxies

Scientific paper

Swift-XRT observations of the X-ray emission from gamma ray bursts (GRBs) and during the GRB afterglow have led to many new results during the past two years. One of these exciting results is that ~1/3-1/2 of GRBs contain detectable X-ray flares. The mean fluence of the X-ray flares is ~10× less than that of the initial prompt emission, but in some cases the flare is as energetic as the prompt emission itself. The flares display fast rises and decays, and they sometimes occur at very late times relative to the prompt emission (sometimes as late as 105 s after T0) with very high peak fluxes relative to the underlying afterglow decay that has clearly begun prior to some flares. The temporal and spectral properties of the flares are found to favor models in which flares arise due to the same GRB internal engine processes that spawned the prompt GRB emission. Therefore, both long and short GRB internal engine models must be capable of producing high fluences in the X-ray band at very late times.

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