Statistical analysis of flux variability and energy spectra of cosmic gamma-ray bursts observed with the BATSE Experiment of the Compton Observatory

Details Statistical analysis of flux variability and energy spectra of cosmic gamma-ray bursts observed with the BATSE Experiment of the Compton Observatory Statistical analysis of flux variability and energy spectra of cosmic gamma-ray bursts observed with the BATSE Experiment of the Compton Observatory

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995azh....72..344m&link_type=abstract

Astronomicheskij Zhurnal, vol. 72, p. 344

Mathematics

Logic

2

Gamma Ray Bursts, Energy Spectra, Statistical Analysis, Particle Flux Density, Cosmic Rays, Astronomical Models, Variability, Astronomical Catalogs

Scientific paper

The results of a statistical study of the flux variability and energy spectra of 260 cosmic gamma-ray bursts in the First catalog of BATSE experiment of the Compton Observatory are presented. It is shown that an averaged flux time history of the bursts has a one-peak asymmetric shape with a steep rising front and a longer decay. Averaged hardness ratio of energy spectra is at maximum at the rising front, and decreases monotonically over the decay part of the averaged time history profile. A comparison of the averaged flux time history profiles of two distinct sets of 'stronger' and 'weaker' bursts has shown that they match closely. On the other hand, the profiles of averaged hardness ratios are widely different: on the average, the stronger bursts are harder than the weaker ones. Based on the observation results, a test of a cosmological model of cosmic gamma-ray bursts was carried out. A close match of the averaged profiles of 'strong' and 'weak' gamma-ray bursts is at odds with that model: a double or triple broadening of profiles of 'weak' bursts, predicted by the cosmological model, cannot be compensated for by the fact that, due to the reddening of photons, the profiles of 'weak' bursts correspond to higher energies of radiated photons having shorter peaks on the flux time history profiles.

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