Volume 564, April 2014
|Number of page(s)||16|
|Published online||10 April 2014|
Simulations of gamma-ray burst afterglows with a relativistic kinetic code
Astronomy Division, Department of Physics,
PO Box 3000, 90014 University of Oulu, Finland
e-mail: email@example.com, firstname.lastname@example.org
2 Physics Department and Columbia Astrophysics Laboratory, Columbia University, 538 West 120th Street, New York, NY 10027, USA
3 Tartu Observatory, 61602 Tõravere, Tartumaa, Estonia
4 Tuorla Observatory, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland
Accepted: 16 February 2014
Aims. This paper introduces a kinetic code that simulates gamma-ray burst (GRB) afterglow emission from the external forward shock and presents examples of some of its applications. One interesting research topic discussed in the paper is the high-energy radiation produced by Compton scattering of the prompt GRB photons against the shock-accelerated electrons. The difference between the forward shock emission in a wind-type and a constant-density medium is also studied, and the emission due to Maxwellian electron injection is compared to the case with pure power-law electrons.
Methods. The code calculates the time-evolving photon and electron distributions in the emission region by solving the relativistic kinetic equations for each particle species. For the first time, the full relativistic equations for synchrotron emission/absorption, Compton scattering, and pair production/annihilation were applied to model the forward shock emission. The synchrotron self-absorption thermalization mechanism, which shapes the low-energy end of the electron distribution, was also included in the electron equation.
Results. The simulation results indicate that inverse Compton scattering of the prompt GRB photons can produce a luminous ≳TeV emission component, even when pair production in the emission region is taken into account. This very high-energy radiation may be observable in low-redshift GRBs. The test simulations also show that the low-energy end of a pure power-law distribution of electrons can thermalize owing to synchrotron self-absorption in a wind-type environment, but without an observable impact on the radiation spectrum. Moreover, a flattening in the forward shock X-ray light curve may be expected when the electron injection function is assumed to be purely Maxwellian instead of a power law. The flux during such a flattening is likely to be lower than the Swift/XRT sensitivity in the case of a constant-density external medium, but a wind environment may result in a higher flux during the shallow decay.
Key words: gamma-ray burst: general / radiation mechanisms: non-thermal / methods: numerical
© ESO, 2014
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