Open AccessA unified treatment of the gamma‐ray burst 021211 and its afterglow
Author(s) -
Kumar Pawan,
Panaitescu Alin
Publication year - 2003
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2003.07138.x
Subject(s) - afterglow , gamma ray burst , physics , ejecta , astrophysics , shock (circulatory) , light curve , astronomy , supernova , medicine
The gamma‐ray burst (GRB) 021211 had a simple light curve, containing only one peak and the expected Poisson fluctuations. Such a burst may be attributed to an external shock, offering the best chance for a unified understanding of the gamma‐ray burst and afterglow emissions. We analyse the properties of the prompt (burst) and delayed (afterglow) emissions of GRB 021211 within the fireball model. Consistency between the optical emission during the first 11 min (which, presumably, comes from the reverse shock heating of the ejecta) and the later afterglow emission (arising from the forward shock) requires that, at the onset of deceleration (∼2 s), the energy density in the magnetic field in the ejecta, expressed as a fraction of the equipartition value (ɛ B ) , is larger than in the forward shock at 11 min by a factor of approximately 10 3 . We find that synchrotron radiation from the forward shock can account for the gamma‐ray emission of GRB 021211; to explain the observed GRB peak flux requires that, at 2 s, ɛ B in the forward shock is larger by a factor 100 than at 11 min. These results suggest that the magnetic field in the reverse shock and early forward shock is a frozen‐in field originating in the explosion and that most of the energy in the explosion was initially stored in the magnetic field. We can rule out the possibility that the ejecta from the burst for GRB 021211 contained more than 10 electron–positron pairs per proton.