The signature of a wind reverse shock in gamma-ray bursts afterglows

A. Pe'er, R. A.M.J. Wijers

Research output: Contribution to journalArticlepeer-review


Explosions of massive stars are believed to be the source of a significant fraction of Gamma-Ray Bursts (GRBs). If this is indeed the case, then the explosion blast wave propagates into a complex density structure, composed of a stellar wind bounded by two shock waves - a wind reverse shock and a forward shock. As the explosion blast wave reaches R0, the radius of the wind reverse shock, it splits into two shock waves - a reverse and a forward shock wave. The reverse shock thus produced is not strong, therefore full analytical treatment is required in calculating its properties. By calculating the dynamics of the flow and the evolution of the blast waves in all of the different stages, we show that the fluid Lorentz factor at r > R0 is equal to 0.725 times the blast wave Lorentz factor as it reaches R0, and is time (and r) independent as long as the blast wave reverse shock exists. Following the calculation of the blast wave evolution, we calculate the radiation expected in different energy bands. We show that about a day after the main explosion, as the blast wave reaches R0, the observed afterglow flux starts to rise. It rises by a factor of about 2 in a few hours, during which the blast wave reverse shock exists, and then declines. We show that the power law index describing light curve time evolution is different at early (before the rise) and late times, and is frequency dependent. We present light curves in the different energy bands for this scenario.

Original languageEnglish
Pages (from-to)1293-1296
Number of pages4
JournalNuovo Cimento della Societa Italiana di Fisica B
Issue number10-11
StatePublished - Oct 2006
Externally publishedYes


Dive into the research topics of 'The signature of a wind reverse shock in gamma-ray bursts afterglows'. Together they form a unique fingerprint.

Cite this