GRBs Radiative Processes: Synchrotron and Synchrotron Self-Absorption From a Power Law Electrons Distribution with Finite Energy Range

Details GRBs Radiative Processes: Synchrotron and Synchrotron Self-Absorption From a Power Law Electrons Distribution with Finite Energy Range GRBs Radiative Processes: Synchrotron and Synchrotron Self-Absorption From a Power Law Electrons Distribution with Finite Energy Range

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1295...87f&link_type=abstract

THE THIRD ALGERIAN WORKSHOP ON ASTRONOMY AND ASTROPHYSICS. AIP Conference Proceedings, Volume 1295, pp. 87-93 (2010).

Astronomy and Astrophysics

Astrophysics

Gamma-Ray Sources (Astronomical), Synchrotron Radiation, Cosmology, Relativistic Electron Beams, Gamma-Ray Sources, Gamma-Ray Bursts, Synchrotron Radiation Instrumentation, Origin And Formation Of The Universe, Relativistic Electron And Positron Beams

Scientific paper

Synchrotron emission behind relativistic magnetic internal-external shocks in gamma-ray bursts cosmological explosions is assumed to be the basic emission mechanism for prompt and afterglow emissions. Inverse Compton from relativistic electrons can also have appreciable effects by upscattering initial synchrotron or blackbody photons or other photons fields up to GeV-TeV energies. For extreme physical conditions such as high magnetic fields (e.g., B>105 Gauss) self-absorption is not negligible and can hardly affect spectra at least for the low energy range. In this paper we present calculations of the synchrotron power, Pν, and their asymptotic forms, generated by a power law relativistic electron distribution of type Ne(γ) = Cγ-p with γ1<γ<γ2, especially for finite values of the higher limit γ2. For this aim we defined the dimensionless parametric function Zp(x,ɛ) with x = ν/ν1 and ɛ = γ2/γ1 so that Pν~Zp(ν/ν1,ɛ), with ν1 = (3/4π)γ12qBsinθ/mc (θ being the pitch angle). Asymptotic forms of this later are derived for three different frequency ranges, i.e., x<<1, 1<>ɛ2. These results are then used to calculate the absorption coefficient, αν, and the source function, Sν, together with their asymptotic forms through the dimensionless parametric functions Hp(x,ɛ) and Yp(x,ɛ), respectively. Further calculation details are also presented and discussed.

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