X-Rays and GeV Flares in GRB Light Curves

Details X-Rays and GeV Flares in GRB Light Curves X-Rays and GeV Flares in GRB Light Curves

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sngh.conf..173g&link_type=abstract

SCIENCE WITH THE NEW GENERATION OF HIGH ENERGY GAMMA-RAY EXPERIMENTS The Variable Gamma-Ray Sources: Their Identifications and C

Computer Science

Scientific paper

Observations are showing that X-ray flares are very common features in GRB light curves. X-ray flares occur from about 100 s up to thousands of seconds after the burst, when the prompt-to-afterglow transition is taking place. In the context of External Shock, X-ray flares are produced by thick shell fireballs emitted by a long duration central engine activity, and represent the beginning of the afterglow emission. The delayed flare photons are expected to interact with the forward shock electrons by Inverse Compton producing high energy counterparts that potentially will be detected by GLAST LAT. Such high energy components could explain the delayed GeV emission detected by EGRET in GRB 940217. Observations with GLAST LAT will give useful information to constrain the origin of X-ray flares.

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