主要内容:
此暴的特点：时标非常短，0.036s，光度低，余辉暗。
精彩摘抄:
 |
| 该短暴的光变 |
 |
| 红点是 GRB 090515所处的位置 |
文章信息:
- · arXiv e-print (arXiv:1007.2185)
- · References in the Article
- · Also-Read Articles (Reads History)
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| Title: |
| The unusual X-ray emission of the short Swift GRB 090515: Evidence for the formation of a magnetar? |
| Authors: |
| Rowlinson, A.; O'Brien, P. T.; Tanvir, N. R.; Zhang, B.; Evans, P. A.; Lyons, N.; Levan, A. J.; Willingale, R.; Page, K. L.; Onal, O.; Burrows, D. N.; Beardmore, A. P.; Ukwatta, T. N.; Berger, E.; Hjorth, J.; Fruchter, A. S.; Tunnicliffe, R. L.; Fox, D. B.; Cucchiara, A. |
| Publication: |
| eprint arXiv:1007.2185 |
| Publication Date: |
| 07/2010 |
| Origin: |
| ARXIV |
| Keywords: |
| Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Extragalactic Astrophysics |
| Comment: |
| 10 pages, 7 figures, MNRAS accepted |
| Bibliographic Code: |
| 2010arXiv1007.2185R |
Abstract
The majority of short gamma-ray bursts (SGRBs) are thought to originate from the merger of compact binary systems collapsing directly to form a black hole. However, it has been proposed that both SGRBs and long gamma-ray bursts (LGRBs) may, on rare occasions, form an unstable millisecond pulsar (magnetar) prior to final collapse. GRB 090515, detected by the Swift satellite was extremely short, with a T_90 of 0.036 +/- 0.016 s, and had a very low fluence of 2 x 10^-8 erg cm^-2 and faint optical afterglow. Despite this, the 0.3 - 10 keV flux in the first 200 s was the highest observed for a SGRB by the Swift X-ray Telescope (XRT). The X-ray light curve showed an unusual plateau and steep decay, becoming undetectable after ~500 s. This behaviour is similar to that observed in some long bursts proposed to have magnetars contributing to their emission. In this paper, we present the Swift observations of GRB 090515 and compare it to other gamma-ray bursts (GRBs) in the Swift sample. Additionally, we present optical observations from Gemini, which detected an afterglow of magnitude 26.4 +/- 0.1 at T+ 1.7 hours after the burst. We discuss potential causes of the unusual 0.3 - 10 keV emission and suggest it might be energy injection from an unstable millisecond pulsar. Using the duration and flux of the plateau of GRB 090515, we place constraints on the millisecond pulsar spin period and magnetic field.
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