Iron line afterglows: How to produce them

Free access article

Issue		Astron. Astrophys. Suppl. Ser. Volume 138, Number 3, September 1999 Gamma-Ray Bursts in the Afterglow Era Contents Rome, November 3-6, 1998


Page(s)		547 - 548
DOI		http://dx.doi.org/10.1051/aas:1999347

DOI: 10.1051/aas:1999347

Astron. Astrophys. Suppl. Ser. 138, 547-548

D. Lazzati^1,2 - S. Campana¹ - G. Ghisellini¹

Correspondence to: lazzati@merate.mi.astro.it

1 - Osservatorio Astronomico di Brera, Via Bianchi 46, I-23807 Merate (Lc), Italy
2 - Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria 16, I-20133 Milano, Italy

Received December 29, 1998; accepted June 9, 1999

Abstract:

We discuss how a powerful iron line emission can be produced if $\sim\! 1-5$ 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.

Key words: gamma-ray: burst

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