Average properties of the time behaviour of gamma-ray bursts
| dc.creator | Stern, Boris | |
| dc.creator | Svensson, Roland | |
| dc.creator | Poutanen, Juri | |
| dc.date | 1997-01-22 | |
| dc.date.accessioned | 2026-07-07T02:22:47Z | |
| dc.date.available | 2026-07-07T02:22:47Z | |
| dc.description | The average peak-aligned profile of all bursts detected by BATSE with sufficient data quality has a simple ``stretched'' exponential shape, F ~ exp[-(t/t_0)^{1/3}], where $t$ is the time measured from the time for the peak flux of the event, and $t_0$ is a time constant. We study the behaviour of $t_0$ of both the post-peak and the pre-peak slopes of the average time profile as a function of the peak brightness range of the burst sample. We found that the post-peak slope shows time dilation when comparing bright and dim bursts, while the pre-peak slope hardly changes. Thus dimmer bursts have a different shape -- they are more asymmetric. This shape-brightness correlation is observed at a 99.6% confidence level. Such a correlation has a natural explanation within the pulse avalanche model, which is briefly described. Complex events, consisting of many pulses are more symmetric and are intrinsically brighter. Bursts consisting of one or a few pulses are intrinsically weaker and more asymmetric. For such a correlation to be observable requires that the luminosity distance distribution of GRBs to be different from a power-law. | |
| dc.description | 5 pages; esa_sp_latex style; 3 postscript figure; Comments to stern@al20.inr.troitsk.ru; to appear in the proceeding of the 2nd INTEGRAL Workshop; St.Malo, France, September 1996 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9701171 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9701171 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/11002 | |
| dc.subject | Astrophysics | |
| dc.title | Average properties of the time behaviour of gamma-ray bursts | |
| dc.type | text |