Unveiling GRB Hard X-ray Afterglow Emission

Details Unveiling GRB Hard X-ray Afterglow Emission Unveiling GRB Hard X-ray Afterglow Emission

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011xau5.confe...2a&link_type=abstract

"The Second Ferrara Workshop on "X-ray Astrophysics up to 511 keV", held in Ferrara (Italy), September 14 - 16, 2011, article #2

Astronomy and Astrophysics

Astrophysics

Scientific paper

Despite the enormous progress occurred in the last 15 years, the Gamma-Ray Bursts (GRB) phenomenon is still far to be fully understood. One of the most important open issues that have still to be settled is the afterglow emission above 10 keV, which is almost completely unexplored. This is due to the lack of sensitive enough detectors operating in this energy band. The only detection, by the BeppoSAX/PDS instrument (15-200 keV), of hard X-ray emission from a GRB (the very bright GRB 990123), combined with optical and radio observations, seriously challenged the standard scenario in which the dominant mechanism is synchrotron radiation produced in the shock of a ultra-relativistic fireball with the ISM, showing the need of a substantial revision of present models. In this respect, next generation X-ray telescopes capable to focus X-rays up to several tens of keV, which will fly in the near future on board the NuSTAR and ASTRO-H missions, and gamma-ray Laue lenses cabable to focus soft gamma-rays up to several hundreds of keV, currently under development, will provide, through follow-up observations of bright GRBs detected and localized by GRB dedicated experiments, an important breakthrough in the GRB field.

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