Synchrotron Self-Compton Model for PKS 2155–304

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...

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Bibliographic Details
Published in:The Astrophysical journal 2008-08, Vol.682 (2), p.784-788
Main Authors: Kusunose, Masaaki, Takahara, Fumio
Format: Article
Language:English
Subjects:
Astronomy
Earth, ocean, space
Exact sciences and technology
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Summary: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 [image]100, the size of the emission region [image]10 super(15) cm, and magnetic field [image]0.1 G explain the observed spectral energy distribution and the flare timescale of [image]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.
ISSN:0004-637X
1538-4357
DOI:10.1086/589233