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Late internal shock model for bright X-ray flares in Gamma-ray Burst afterglows and GRB 011121 | | Y. Z. Fan
; D. M. Wei
; | | Date: |
8 Jun 2005 | | Subject: | astro-ph | | Affiliation: | PMO and Unlv) and D. M. Wei (PMO | | Abstract: | We explore two possible models which might give rise to bright X-ray flares in GRBs afterglows. One is an external forward-reverse shock model, in which the shock parameters of forward/reverse shocks are taken to be quite different. The other is a so called "late internal shock model", which requires a refreshed unsteady relativistic outflow generated after the prompt $gamma-$ray emission. In the forward-reverse shock model, after the time $t_ imes$ at which the RS crosses the ejecta, the flux declines more slowly than $(t_oplus/t_ imes)^{-(2+eta)}$, where $t_oplus$ denotes the observer’s time and $eta$ is the spectral index of the X-ray emission. In the ``late internal shock model", decaying slopes much steeper than $(t_oplus/t_{
m e, oplus})^{-(2+eta)}$ are possible if the central engine shuts down after $t_{
m e, oplus}$ and the observed variability timescale of the X-ray flare is much shorter than $t_{
m e, oplus}$. The sharp decline of the X-ray flares detected in GRB 011121, XRF 050406, GRB 050502b, and GRB 050730 rules out the external forward-reverse shock model directly and favors the "late internal shock model". These X-ray flares could thus hint that the central engine operates again and a new unsteady relativistic outflow is generated just a few minutes after the intrinsic hard burst. | | Source: | arXiv, astro-ph/0506155 | | Services: | Forum | Review | PDF | Favorites | |
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