ar X iv : a st ro - p h / 02 05 14 4 v 2 1 9 Ju n 20 02 X - ray Rich GRB , Photospheres and Variability
نویسندگان
چکیده
We investigate the relationship between the quasi-thermal baryon-related photosphere in relativistic outflows, and the internal shocks arising outside them, which out to a limiting radius may be able to create enough pairs to extend the optically thick region. Variable gamma-ray light curves are likely to arise outside this limiting pair-forming shock radius, while X-ray excess bursts may arise from shocks occurring below it; a possible relation to X-ray flashes is discussed. This model leads to a simple physical interpretation of the observational gamma-ray variability-luminosity relation.
منابع مشابه
ar X iv : a st ro - p h / 02 05 14 4 v 1 9 M ay 2 00 2 X - ray Rich GRB , Photospheres and Variability
We investigate the relationship between the quasi-thermal baryon-related photosphere in relativistic outflows, and the internal shocks arising outside them, which out to a limiting radius may be able to create enough pairs to extend the optically thick region. Variable gamma-ray light curves are likely to arise outside this limiting pair-forming shock radius, while X-ray excess bursts may arise...
متن کاملar X iv : a st ro - p h / 02 06 42 3 v 1 2 4 Ju n 20 02 EARLY GRB AFTERGLOWS REVISITED
The standard afterglow model neglects the presence of the GRB prompt radiation ahead of the blast wave. In fact, the blast wave is dramatically influenced by the leading gamma-ray front which preaccelerates the ambient medium and loads it with electron-positron pairs. The front sweeps the medium outward with a high Lorentz factor and results in a spectacular effect: the GRB ejecta moves freely ...
متن کاملar X iv : a st ro - p h / 03 06 28 4 v 2 1 4 Ju n 20 03 Delayed soft X - ray emission lines in the afterglow of GRB 030227
Strong, delayed X-ray line emission is detected in the afterglow of GRB 030227, appearing near the end of the XMM-Newton observation, nearly twenty hours after the burst. The observed flux in the lines, not simply the equivalent width, sharply increases from an undetectable level (< 1.7 × 10 −14 erg cm −2 s −1 , 3σ) to 4.1 +0.9 −1.0 × 10 −14 erg cm −2 s −1 in the final 9.7 ks. The line emission...
متن کامل