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- W3100286860 abstract "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 ~100, the size of the emission region ~1015 cm, and magnetic field ~0.1 G explain the observed spectral energy distribution and the flare timescale of ~a few minutes. This model with a large value of Γ 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." @default.
- W3100286860 created "2020-11-23" @default.
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- W3100286860 date "2008-08-01" @default.
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- W3100286860 title "Synchrotron Self‐Compton Model for PKS 2155−304" @default.
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- W3100286860 doi "https://doi.org/10.1086/589233" @default.
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