Radio constraints on shell afterglow theories

Details Radio constraints on shell afterglow theories Radio constraints on shell afterglow theories

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aipc..428..727b&link_type=abstract

Fourth Huntsville gamma-ray burst symposium. AIP Conference Proceedings, Volume 428, pp. 727-731 (1998).

Physics

1

Gamma-Ray Sources, Gamma-Ray Bursts, Radiation Mechanisms, Polarization

Scientific paper

The radio afterglow from GRB970508 places strong constraints on the gamma-ray burst energetics. In this article, I discuss the constraint on the total energy in the gamma-ray burst if the afterglow is optically thick synchrotron emission from a relativistic shell that sweeps up interstellar gas. It is found that if the shell cools rapidly as it expands, then the gamma-ray burst must contain of order a solar rest mass energy or more to produce the radio emission. If none of the energy is radiated, then the energy in the gamma-ray burst is much larger than the observed gamma-ray fluence of 2×1051 ergs, the source diameter must be larger than the inferred 3 μarcsec, and >20% must end up in the electrons at the time of the radio emission. Some of these limits can be circumvented by allowing a short period of efficient cooling.

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