Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aipc..836..253d&link_type=abstract
GAMMA-RAY BURSTS IN THE SWIFT ERA: Sixteenth Maryland Astrophysics Conference. AIP Conference Proceedings, Volume 836, pp. 253-
Astronomy and Astrophysics
Astrophysics
Gamma-Ray Sources, Gamma-Ray Bursts, X-Ray Sources, X-Ray Bursts
Scientific paper
Gamma-Ray Bursts (GRBs) are widely thought to originate from collimated jets of material moving at relativistic velocities. Emission from such a jet should be visible even when viewed from outside the angle of collimation. Such off-jet emission has been proposed as an explanation for X-Ray Flashes (XRFs). I summarize recent work on the special relativistic transformation of the burst quantities Eiso and Epeak as a function of viewing angle, in the context the top-hat shaped variable opening-angle jet model. The resulting formulae serve as input for a Monte Carlo population synthesis method. I find that the XRFs seen by HETE-2 and BeppoSAX cannot be easily explained as classical GRBs viewed off-jet. For γ < 300, such models predict a large population of observable off-jet bursts that lie away from the is Epeak ~ Eiso1/2 relation. An inverse correlation between γ and Ω0 has the effect of greatly reducing the visibility of off-jet events. Therefore, unless γ > 300 for all bursts or unless there is a strong inverse correlation between γ and Ω0, top-hat variable opening-angle jet models produce a significant population of bursts away from the Epeak ~ Eiso1/2 and Epeak ~ Eγβ relations, in contradiction of current observations.
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