Astron. Astrophys. Suppl. Ser.
Volume 138, Number 3, September 1999Gamma-Ray Bursts in the Afterglow Era Contents Rome, November 3-6, 1998
|Page(s)||527 - 528|
|Published online||15 September 1999|
Quasi–thermal comptonization and GRBs
Osservatorio Astronomico di Brera, via Bianchi 46, I-23807 Merate, Italy
2 S.I.S.S.A., via Beirut 2-4, I-34014, Italy
Accepted: 26 January 1999
Quasi–thermal Comptonization in internal shocks formed between relativistic shells can account for the high energy emission of gamma–ray bursts (GRB). This is the dominant cooling mechanism if the typical energy of the emitting particles is achieved either through the balance between heating and cooling or as a result of electron–positron (e) pair production. Both processes yield sub/mildly relativistic energies. In this case the synchrotron spectrum is self–absorbed, providing the seed photons for the Comptonization process, whose spectrum is flat [ const] , ending either in an exponential cutoff or a Wien peak.
Key words: gamma rays: bursts / radiation mechanisms: non–thermal, thermal / X-rays: general
© European Southern Observatory (ESO), 1999