Iron line afterglows: how to produce them
arXiv:astro-ph/9906235 · doi:10.1051/aas:1999347
Abstract
We discuss how a powerful iron line emission can be produced if ~1-5 iron rich solar masses are concentrated in the close vicinity of the burst. Recombination, thermal and fluorescent reflection are discussed. We find that recombination suffers the high Compton temperature of the plasma while the other two scenarios are not mutually exclusive and could account for the claimed iron line detected in two afterglows.
arXiv comment2 pages, A&AS in press, proceedings of the Workshop "Gamma Ray Bursts in the Afterglow Era" held in Rome, November 1998