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H.E.S.S. observed TeV blazar PKS 2155--304 in a strong flare state in 2006July. The TeV flux varied on timescale as short as a few minutes, which setsstrong constraints on the properties of the emission region. By use of thesynchrotron self-Compton model, we found that models with the bulk Lorentzfactor $\sim 100$, the size of the emission region $\sim 10^{15}$ cm, andmagnetic field $\sim 0.1$ G explain the observed spectral energy distributionand 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 alsoin the X-ray band. The major cooling process of electrons/positrons in the jetis inverse Compton scattering off synchrotron photons. The energy content ofthe jet is highly dominated by particle kinetic energy over magnetic energy.

Synchrotron Self-Compton Model for PKS 2155-304