Sari, R. and Piran, T. (1999) The early afterglow. Astronomy and Astrophysics Supplement Series, 138 (3). pp. 537-538. ISSN 0365-0138. doi:10.1051/aas:1999342. https://resolver.caltech.edu/CaltechAUTHORS:20180413-132411191
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Abstract
We calculate the expected spectrum and light curves of the early afterglow. For short GRBs the peak of the afterglow will be delayed, typically, by few dozens of seconds after the burst. The X-ray and γ-ray characteristics of this delayed emission provide a way to discriminate between late internal shocks emission (part of the GRB) and the early afterglow signal. Detection of this delayed emission will prove the internal shock scenario as producing the GRB, and will pinpoint the initial Lorentz factor . In the optical band, the dominant emission arises from the reverse shock. This shock, carries a comparable amount of energy to the forward shock. It radiates this energy at much lower frequencies, producing a short optical flash of 15th magnitude or brighter.
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| Additional Information: | © European Southern Observatory (ESO), 1999. Received December 29; accepted December 29, 1998. This research was supported by the US-Israel BSF 95-328 and by a grant from the Israeli Space Agency. R.S. thanks the Sherman Fairchild Foundation for support. | ||||||||
| Group: | TAPIR | ||||||||
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| Issue or Number: | 3 | ||||||||
| DOI: | 10.1051/aas:1999342 | ||||||||
| Record Number: | CaltechAUTHORS:20180413-132411191 | ||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20180413-132411191 | ||||||||
| Official Citation: | The early afterglow R. Sari and T. Piran Astron. Astrophys. Suppl. Ser., 138 3 (1999) 537-538 DOI: https://doi.org/10.1051/aas:1999342 | ||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||
| ID Code: | 85838 | ||||||||
| Collection: | CaltechAUTHORS | ||||||||
| Deposited By: | George Porter | ||||||||
| Deposited On: | 13 Apr 2018 20:43 | ||||||||
| Last Modified: | 15 Nov 2021 20:32 |
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