Astronomy and Astrophysics – Astrophysics – Cosmology and Extragalactic Astrophysics
Scientific paper
2009-02-04
Astronomy and Astrophysics
Astrophysics
Cosmology and Extragalactic Astrophysics
Revised version accepted for publication in MNRAS
Scientific paper
The jets of powerful blazars propagate within regions relatively dense of radiation produced externally to the jet. This radiation is a key ingredient to understand the origin of the high energy emission of blazars, from the X-ray to the gamma-ray energy band. These external radiation fields control the amount of the inverse Compton radiation with respect to the synchrotron flux. Therefore the predicted spectral energy distribution (SED) will depend on where the jet dissipates part of its energy to produce the observed radiation. We investigate in detail how the SED changes as a function of the location of the jet dissipation region, by assuming rather "standard" (i.e. "canonical") prescriptions for the accretion disk and its X-ray corona, the profile of the jet magnetic field and the external radiation. The magnetic energy density of a "canonical" jet almost never dominates the radiative cooling of the emitting electrons, and consequently the inverse Compton flux almost always dominates the bolometric output. This is more so for large black hole masses. Dissipation taking place beyond the broad line region is particularly interesting, since it accounts in a simple way for the largest inverse Compton to synchrotron flux ratios accompanied by an extremely hard X-ray spectrum. Furthermore it makes the high power blazars at high redshift useful tools to study the optical to UV cosmic backgrounds.
Ghisellini Gabriele
Tavecchio Fabrizio
No associations
LandOfFree
Canonical high power blazars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Canonical high power blazars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Canonical high power blazars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-25173