Synchrotron self-Compton flaring of TeV blazars. II. Linear and nonlinear electron cooling

Details Synchrotron self-Compton flaring of TeV blazars. II. Linear and nonlinear electron cooling Synchrotron self-Compton flaring of TeV blazars. II. Linear and nonlinear electron cooling

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009a%26a...503..309r&link_type=abstract

Astronomy and Astrophysics, Volume 503, Issue 2, 2009, pp.309-322

Astronomy and Astrophysics

Astrophysics

2

Radiation Mechanisms: Non-Thermal, Methods: Analytical, Galaxies: Active

Scientific paper

A theoretical radiation model for the flaring of TeV blazars is discussed here for the case of a nonlinear electron synchrotron cooling in these sources. We compute analytically the optically thick and thin synchrotron radiation intensities and photon density distributions in the emission knot as functions of frequency and time followed by the synchrotron self-Compton intensity and fluence in the optically thin frequency range using the Thomson approximation of the inverse Compton cross section. At all times and frequencies, the optically thin part of the synchrotron radiation process is shown to provide the dominant contribution to the synchrotron self-Compton quantities, while the optically thick part is always negligible. Afterwards, we compare the linear to the nonlinear synchrotron radiation cooling model using the data record of PKS 2155-304 on MJD 53944 favouring a linear cooling of the injected monoenergetic electrons. The good agreement of both the linear and the nonlinear cooling model with the data supports the relativistic pickup process operating in this source. Additionally, we discuss the synchrotron self-Compton scattering, applying the full Klein-Nishina cross section to achieve the most accurate results for the synchrotron self-Compton intensity and fluence distributions.

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