High-Energy Gamma-Rays from GRB X-ray Flares

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dc.creatorWang, Xiang-Yu
dc.creatorLi, Zhuo
dc.creatorMeszaros, Peter
dc.date2007-02-23
dc.date.accessioned2026-07-07T10:36:52Z
dc.date.available2026-07-07T10:36:52Z
dc.descriptionThe recent detection of X-ray flares during the afterglow phase of gamma-ray bursts (GRBs) suggests an inner-engine origin, at radii inside the forward shock. There must be inverse Compton (IC) emission arising from such flare photons scattered by forward shock afterglow electrons when they are passing through the forward shock. We find that this IC emission produces high energy gamma-ray flares, which may be detected by AGILE, GLAST and ground-based TeV telescopes. The anisotropic IC scattering between flare photons and forward shock electrons does not affect the total IC component intensity, but cause a time delay of the IC component peak relative to the flare peak. The anisotropic scattering effect may also weaken, to some extent, the suppression effect of the afterglow intensity induced by the enhanced electron cooling due to flare photons. We speculate that this IC component may already have been detected by EGRET from a very strong burst--GRB940217. Future observations by GLAST may help to distinguish whether X-ray flares originate from late central engine activity or from external shocks.
dc.description4 pages, Contributed talk presented at "The First GLAST Symposium", Feb.5-8 2007, Stanford University
dc.identifierhttps://arxiv.org/abs/astro-ph/0702617
dc.identifierhttp://arxiv.org/abs/astro-ph/0702617
dc.identifierAIPConf.Proc.921:271-273,2007
dc.identifierdoi:10.1063/1.2757320
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/180200
dc.subjectAstrophysics
dc.titleHigh-Energy Gamma-Rays from GRB X-ray Flares
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