Volume 415, Number 2, February IV 2004
|Page(s)||443 - 450|
|Published online||11 February 2004|
Reconsidering the origin of the X-ray emission lines in GRB 011211
INAF–Osserv. Astron. di Brera, via Bianchi 46, 23807 Merate, Italy
2 Institute of Astronomy, University of Cambridge, Madingley Road, CB3 0HA Cambridge, UK
Corresponding author: F. Tavecchio, email@example.com
Accepted: 29 September 2003
We reanalyze the XMM–Newton data of GRB 011211 showing that the spectral features, interpreted by Reeves et al. ([CITE], [CITE]) as due to thermal emission from a collisionally ionized plasma, can be also reproduced by a reflection model (with ionization parameter ). We discuss the implications of this interpretation, estimating the total mass required in the simplified case of a funnel geometry. We conclude that a moderate clumping of the reprocessing material (corresponding to a filling factor of the order of ) is required. Finally we show that, if this interpretation is correct, a bright quasi–thermal component is expected in the optical–UV band (containing about of the luminosity of the illuminating continuum), whose presence can be used to test the reflection model.
Key words: gamma rays: bursts / line: formation / radiation mechanisms: general
© ESO, 2004
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.