Gamma Ray Bursts in Pulsar Wind Bubbles: Observational implications

Details Gamma Ray Bursts in Pulsar Wind Bubbles: Observational implications Gamma Ray Bursts in Pulsar Wind Bubbles: Observational implications

2003-02-14

arxiv.org/abs/astro-ph/0302282v1

Astronomy and Astrophysics

Astrophysics

4 pages, contributed talk at the meeting "Gamma Ray Bursts in the Afterglow Era - Third Workshop", September 2002, Rome, Italy

Scientific paper

We present the main observational features expected for Gamma-Ray Bursts (GRBs) that occur inside pulsar wind bubbles (PWBs). This is the most natural outcome of the supranova model, where initially a supernova (SN) explosion takes place, leaving behind a supra-massive neutron star, which loses its rotational energy over a time t_sd and collapses to a black hole, triggering a GRB. We find that the time delay, t_sd, between the SN and GRB events is the most important parameter that determines the behavior of the system. We consider the afterglow, prompt GRB and PWB emission. Constraints on the model are derived for a spherical PWB, from current afterglow observations and the lack of direct detection of the PWB emission. We find that a simple spherical model cannot account for the X-ray features detected in some afterglows, together with the typical afterglow emission that was observed for the same GRBs. The discrepancies with observations may be reconciled by resorting to a non-spherical geometry, where the PWB is elongated along the polar axis. Finally, we predict that the inverse Compton upscattering of PWB photons by the relativistic electrons of the afterglow (external Compton) should lead to high energy emission during the early afterglow that may explain the GeV photons detected by EGRET for a few GRBs, and should be detectable by future missions such as GLAST.

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