Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/26399
Title: The dust scattering model cannot explain the shallow X-ray decay in GRB afterglows
Authors: Shen, R-F.
Kumar, P.
Willingale, R.
O'Brien, P. T.
Evans, P. A.
First Published: 21-Feb-2009
Publisher: Oxford University Press
Citation: Monthly Notices of the Royal Astronomical Society, 2009, 393 (2), pp. 598-606
Abstract: A dust scattering model was recently proposed to explain the shallow X-ray decay (plateau) observed prevalently in Gamma-Ray Burst (GRB) early afterglows. In this model, the plateau is the scattered prompt X-ray emission by the dust located close (about 10 to a few hundred pc) to the GRB site. In this paper, we carefully investigate the model and find that the scattered emission undergoes strong spectral softening with time, due to the model's essential ingredient that harder X-ray photons have smaller scattering angle thus arrive earlier, while softer photons suffer larger angle scattering and arrive later. The model predicts a significant change, that is Δβ∼ 2–3, in the X-ray spectral index from the beginning of the plateau towards the end of the plateau, while the observed data show close to zero softening during the plateau and the plateau-to-normal transition phase. The scattering model predicts a big difference between the harder X-ray light curve and the softer X-ray light curve, i.e. the plateau in harder X-rays ends much earlier than in softer X-rays. This feature is not seen in the data. The large scattering optical depths of the dust required by the model imply strong extinction in optical, A[subscript: V]≳ 10, which contradicts current findings of A[subscript: V]= 0.1–0.7 from optical and X-ray afterglow observations. We conclude that the dust scattering model cannot explain the X-ray plateaus.
DOI Link: 10.1111/j.1365-2966.2008.14223.x
ISSN: 0035-8711
eISSN: 1365-2966
Links: http://hdl.handle.net/2381/26399
http://mnras.oxfordjournals.org/content/393/2/598
Version: Publisher Version
Type: Journal Article
Rights: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2009 The Authors. Journal compilation © 2009 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Deposited with reference to the publisher’s open access archiving policy.
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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