However, episodes of rapid flares as recently reported at TeV energies are beyond the reach of the single component SSC model with one dominant varying parameter. Stronger -ray flares observed in some HBLs like Mrk 501 are understood in terms of additional, smooth increases also of the emitting electron density. In the Klein-Nishina regime the model predicts for HBLs lower inverse Compton fluxes relative to synchrotron, and milder -ray relative to X-ray variations. We find relations among spectral parameters of the IC radiation in both the Thomson (for Low energy BL Lacs) and the Klein-Nishina regimes (mainly for High energy BL Lacs) whence we compute how variability is driven by a smooth increase of key source parameters, primarily the root mean square electron energy. We start from the homogeneous single-zone SSC source model, with log-parabolic energies distributions of emitting electron as required by the X-ray data of many sources.
From the observed correlations among the spectral parameters (peak frequencies, fluxes and curvature) during optical/X-ray variations we aim at predicting corresponding correlations in the -ray band, and the actual relations between the -ray and the X-ray variability consistent with the SSC emission process. Rays relative to the optical/X rays might be surmised to be enhanced in BL Lacs as these photons are upscattered via the inverse Compton (IC) process.Īims. This subclass of Active Galactic Nuclei is marked by non-thermal beamed radiations, highly variable on timescales of days or less. The synchrotron-self Compton (SSC) radiation process is widely held to provide a close representation of the double peaked spectral energy distributions from BL Lac Objects (BL Lacs). Received 31 March 2009 / Accepted 12 July 2009Ĭontext. INAF, via Fosso del Cavaliere 1, 00100 Roma, Italy Harvard, Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USA SSC radiation in BL Lacertae sources, the end of the tetherĪ. Paggi 1 - F. Massaro 2 - V. Vittorini 3 - A. Cavaliere 1 - F. D'Ammando 1,3 - F. Vagnetti 1 - M. Tavani 1,3ġ - Dipartimento di Fisica, Università di Roma Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma, Italy Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences
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