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Iron line afterglows: how to produce them

Davide Lazzati·Sergio Campana·Gabriele Ghisellini
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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.

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Davide Lazzati, Sergio Campana, Gabriele Ghisellini. 1999-06-14. Iron line afterglows: how to produce them. https://doi.org/10.1051/aas%3A1999347

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