GeV emission from short gamma-ray bursts: the case of GRB 081024B
A. Corsi1,2⋆, D. Guetta3 and L. Piro2
Università degli studi di Roma “Sapienza” and INFN-Sezione di
Piazzale Aldo Moro 2,
2 INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Roma, via Fosso del Cavaliere 100, 00133 Roma, Italy
3 INAF - Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio Catone, Italy
Accepted: 26 August 2010
Aims. We investigate whether the high energy tail detected by the Fermi/LAT for the short GRB 081024B can be caused by synchrotron and self-Compton emission in the context of either the internal or external shock models.
Methods. For the internal shock scenario, we explore the possibility of generating the high energy photons directly by means of the synchrotron process, or inverse Compton emission in which target photons are synchrotron photons produced in internal shocks taking place in a lately emitted shell (delayed internal shocks). In the external shock scenario, we test whether the high energy tail can be an extension of the afterglow synchrotron emission, or alternatively the inverse Compton component associated with the afterglow synchrotron photons.
Results. For the internal shock scenario, we conclude that only an inverse Compton component from delayed internal shocks can explain the high energy tail that extends to the GeV range. In the external shock scenario, we show that the high energy tail may be interpreted as synchrotron afterglow emission, if the slow cooling phase starts as early as a few seconds after the trigger. On the other hand, the observed high energy tail is consistent with an inverse Compton component of the afterglow in the fast cooling regime.
Key words: gamma-rays burst: individual: GRB 081024B / X-rays: individuals:GRB 081024B / X-rays: bursts / radiation mechanisms: non-thermal
© ESO, 2010