主要内容:
暗一些，时间长一些，但是总能量还是很大。而且有的甚至到一个月以后。
精彩摘抄:
 |
| 能量 |
 |
| 光度 |
文章信息:
- · arXiv e-print (arXiv:1004.3831)
- · References in the Article
- · Also-Read Articles (Reads History)
- ·
- · Translate This Page
Abstract
We complete the flare observational picture analysing the late time (i.e. t_{pk} >~ 1000 s) flares observed by Swift in the 0.3-10 keV energy band. The aim is to extend the knowledge of the temporal and energetic properties of X-ray flares up to 3 orders of magnitude in time in order to identify possible differences in the mechanism producing the early and late time flaring emission, if any. This requires the complete understanding of the observational biases affecting the detection of X-ray flares superimposed on a fading continuum at t > 1000 s. We find that the width of flares increases with time up to 10^6 s, and the linear relation between decay time and rise time still holds for late time flares. Late time flares are less energetic than early time flares by at least 1 order of magnitude, and they are also dimmer, being the peak luminosity anticorrelated with the peak time. Whatever produces each X-ray flare keeps memory of the previous GRB history, starting from the prompt emission, and it has to be capable to release huge (~ 10^50 erg) amount of energy up to 1 month after the main event. These results, together with related works on early time flares and bright flares, provide a set of clear observational properties that every model aiming at explaining the GRB emission has to face.
没有评论:
发表评论