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|Title:||The signature of supernova ejecta in the X-ray afterglow of the gamma-ray burst 011211|
|Authors:||Reeves, J. N.|
Osborne, Julian P.
Pounds, Kenneth A.
O'Brien, Paul T.
Short, A. D. T.
Turner, Martin J. L.
Watson, Michael G.
Mason, K. O.
|Publisher:||Nature Publishing Group|
|Citation:||Nature, 2002, 416, pp.512-515|
|Abstract:||Now that γ-ray bursts (GRBs) have been determined to lie at cosmological distances, their isotropic burst energies are estimated to be as high as 10[superscript 54] erg (ref. 2), making them the most energetic phenomena in the Universe. The nature of the progenitors responsible for the bursts remains, however, elusive. The favoured models range from the merger of two neutron stars in a binary system[superscript 3-5] to the collapse of a massive star[superscript 6-8]. Spectroscopic studies of the afterglow emission could reveal details of the environment of the burst, by indicating the elements present, the speed of the outflow and an estimate of the temperature. Here we report an X-ray spectrum of the afterglow of GRB011211, which shows emission lines of magnesium, silicon, sulphur, argon, calcium and possibly nickel, arising in metal-enriched material with an outflow velocity of the order of one-tenth the speed of light. These observations strongly favour models[superscript 30] where a supernova explosion from a massive stellar progenitor precedes the burst event and is responsible for the outflowing matter.|
|Rights:||Copyright © 2002 Macmillan Magazines Ltd. Deposited with reference to the publisher’s archiving policy available on the SHERPA/RoMEO website.|
|Appears in Collections:||Published Articles, Dept. of Physics and Astronomy|
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|10.1038_416512a.pdf||Post-review (final submitted)||217.58 kB||Adobe PDF||View/Open|
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