主要内容:
Contain many X-ray data and E_peak, E_iso, spectral index, while mainly is the temporal properties.
精彩摘抄:
Partial data
composite plot of XRF and C-GRB.
Sketch of C-GRB(classical GRB) and XRF light curves
文章信息:
- arXiv e-print (arXiv:0801.4319)
- · References in the Article
- ·
- · Translate This Page
| Title: |
| Global Properties of X-Ray Flashes and X-Ray-Rich Gamma-Ray Bursts Observed by Swift |
| Authors: |
| Sakamoto, T.; Hullinger, D.; Sato, G.; Yamazaki, R.; Barbier, L.; Barthelmy, S. D.; Cummings, J. R.; Fenimore, E. E.; Gehrels, N.; Krimm, H. A.; Lamb, D. Q.; Markwardt, C. B.; Osborne, J. P.; Palmer, D. M.; Parsons, A. M.; Stamatikos, M.; Tueller, J. |
| Publication: |
| eprint arXiv:0801.4319 |
| Publication Date: |
| 01/2008 |
| Origin: |
| ARXIV |
| Keywords: |
| Astrophysics |
| Comment: |
| 50 pages, 22 figures, Accepted for publication in ApJ |
| Bibliographic Code: |
| 2008arXiv0801.4319S |
Abstract
We describe and discuss the spectral and temporal characteristics of the prompt emission and X-ray afterglow emission of X-ray flashes (XRFs) and X-ray-rich gamma-ray bursts (XRRs) detected and observed by Swift between December 2004 and September 2006. We compare these characteristics to a sample of conventional classical gamma-ray bursts (C-GRBs) observed during the same period. We confirm the correlation between Epeak_obs and fluence noted by others and find further evidence that XRFs, XRRs and C-GRBs form a continuum. We also confirm that our known redshift sample is consistent with the correlation between the peak energy in the GRB rest frame (Epeak_src) and the isotropic radiated energy (Eiso), so called the Epeak_src-Eiso relation. The spectral properties of X-ray afterglows of XRFs and C-GRBs are similar, but the temporal properties of XRFs and C-GRBs are quite different. We found that the light curves of C-GRB afterglows show a break to steeper indices (shallow-to-steep break) at much earlier times than do XRF afterglows. Moreover, the overall luminosity of XRF X-ray afterglows is systematically smaller by a factor of two or more compared to that of C-GRBs. These distinct differences between the X-ray afterglows of XRFs and C-GRBs may be the key to understanding not only the mysterious shallow-to-steep break in X-ray afterglow light curves, but also the unique nature of XRFs.
没有评论:
发表评论