GRB 090510: Early LAT Emission is not from External Shock

Details GRB 090510: Early LAT Emission is not from External Shock GRB 090510: Early LAT Emission is not from External Shock

Aug 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aipc.1358..191h&link_type=abstract

GAMMA RAY BURSTS 2010. AIP Conference Proceedings, Volume 1358, pp. 191-194 (2011).

Astronomy and Astrophysics

Astronomy

Gamma-Ray Sources (Astronomical), Shock Waves, Redshift, Spectral Analysis, Gamma-Ray Sources, Gamma-Ray Bursts, Planetary Bow Shocks, Interplanetary Shocks, Distances, Redshifts, Radial Velocities, Spatial Distribution Of Galaxies, Luminosities, Magnitudes, Effective Temperatures, Colors, And Spectral Classification

Scientific paper

Long-lived high-energy (>100 MeV) emission, a common feature of most Fermi-LAT detected gamma-ray burst, is detected up to ~102 s in the short GRB 090510. We study the origin of this long-lived high-energy emission, using broad-band observations including X-ray and optical data. We confirm that the late >100 MeV, X-ray and optical emission can be naturally explained via synchrotron emission from an adiabatic forward shock propagating into a homogeneous ambient medium with low number density under significant Klein-Nishina effects. Under the constraints from the low-energy observations, the adiabatic forward shock synchrotron emission is consistent with the later-time (t>2 s) high-energy emission, but falls below the early-time (t<2 s) high energy emission. Thus we argue that an extra high energy component is needed at early times. A standard reverse shock origin is found to be inconsistent with this extra component. Therefore, we attribute the early part of the high-energy emission (t<2 s) to the prompt component, and the long-lived high energy emission (t>2 s) to the adiabatic forward shock synchrotron afterglow radiation. This avoids the requirement for an extremely high initial Lorentz factor.

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