The flux- E p relation within GRB060218 in comparison with typical GRB pulses

Details The flux- E p relation within GRB060218 in comparison with typical GRB pulses The flux- E p relation within GRB060218 in comparison with typical GRB pulses

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010scchg..53s..78d&link_type=abstract

Science China Physics, Mechanics and Astronomy, Volume 53, Issue 1, pp.78-81

Astronomy and Astrophysics

Astronomy

1

Gamma-Ray Bursts, Gamma-Rays Observations, High-Energy Phenomenon, Radiation Mechanism

Scientific paper

The prompt gamma-ray/X-ray emission of gamma-ray burst (GRB) 060218 was simultaneously observed by the Burst Alert Telescope (BAT) and X-ray Telescope (XRT) onboard Swift. Its peak energy of the joint vf v spectrum ( E p) clearly evolves with time from tens of keV to ˜1 keV, crossing both the BAT and XRT bands. The best fit yields log E p=(4.61±0.23)+(-1.29±0.08) log t, with a correlation coefficient of 0.98 and a chance probability of p<10-4. We derive its bolometric flux ( F) in the 0.01-104 keV band, and find that its F-E p relation, with a power-law index of 0.37, is much shallower than that observed in typical GRB pulses. Discussion of this shallowness is presented.

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