Synchrotron Self-Compton Model for PKS 2155-304

Details Synchrotron Self-Compton Model for PKS 2155-304 Synchrotron Self-Compton Model for PKS 2155-304

2008-07-24

arxiv.org/abs/0807.3773v1

Astronomy and Astrophysics

Astrophysics

9 pages, 5 figures, 2 tables, to appear in the Astrophysical Journal, Vol. 682

Scientific paper

10.1086/589233

H.E.S.S. observed TeV blazar PKS 2155--304 in a strong flare state in 2006 July. The TeV flux varied on timescale as short as a few minutes, which sets strong constraints on the properties of the emission region. By use of the synchrotron self-Compton model, we found that models with the bulk Lorentz factor $\sim 100$, the size of the emission region $\sim 10^{15}$ cm, and magnetic field $\sim 0.1$ G explain the observed spectral energy distribution and the flare timescale $\sim$ a few minutes. This model with a large value of $\Gamma$ accounts for the emission spectrum not only in the TeV band but also in the X-ray band. The major cooling process of electrons/positrons in the jet is inverse Compton scattering off synchrotron photons. The energy content of the jet is highly dominated by particle kinetic energy over magnetic energy.

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