Canonical high power blazars
By G. Ghisellini, F. Tavecchio. 2009
398 citations recorded by the source corpus.
The jets of powerful blazars propagate within regions relatively dense of radiation produced externally to the jet. This radiation is a key ingredient to u nderstand the origin of the high energy emission of blazars, from the X‐ray to the γ‐ray energy band. The main components contributing to the external radiation field are the accreti on disk emission, including its X‐ray corona, the broad line region, the infrared emitting torus a nd the cosmic background radiation. Their importance changes as a function of the distance from the black hole and of the value of the bulk Lorentz factor of the jet. These external ra diation 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 ra ther “standard” (i.e. “canonical”) prescriptions for the accretion disk and its X‐ray corona, t he profile of the jet magnetic field and the external radiation. We confirm that most of the dissip ation, if producing the γ‐ray flux we see, must occur at hundreds of Schwarzschild radii fro m the black hole, to avoid the γ‐γ! e ± process, and the consequent re‐emission by the produced pairs. 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 acc ounts 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.
Subfields: Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/6d23ede03f8d40264315f6288ea6b06c2e054eaa
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Citations in the corpus
- RADIO-LOUD NARROW-LINE SEYFERT 1 AS A NEW CLASS OF GAMMA-RAY ACTIVE GALACTIC NUCLEI (2009, methodology): “As for PMN J0948+0022, these SEDs show clear similarities with blazars and therefore we fitted them with the synchrotron and inverse-Compton model developed by Ghisellini & Tavecchio (2009).”
- Detection of significant cm to sub-mm band radio and γ-ray correlated variability in Fermi bright blazars (2014, background): “…would then be produced in the shocks by IC up-scattering of ambient photons from the accretion disk, BLR, dusty torus and/or jet (Synchrotron Self-Compton) depending on the shock location and available ambient photon fields and their radiation energy densities (e.g. Ghisellini & Tavecchio 2009).”
- The transition between BL Lac objects and flat spectrum radio quasars (2010, background): “It isa one– zone, leptonic model, fully discussed in Ghisellini & Tavecchio (2009).”
- TURBULENT, EXTREME MULTI-ZONE MODEL FOR SIMULATING FLUX AND POLARIZATION VARIABILITY IN BLAZARS (2013, background): “The high γ-ray to X-ray flux ratio is one reason why seed photons from thermal emission from broad emission-line clouds and a dusty torus is favored by many authors (e.g., Ghisellini & Tavecchio 2009).”
- FERMI/LARGE AREA TELESCOPE DISCOVERY OF GAMMA-RAY EMISSION FROM A RELATIVISTIC JET IN THE NARROW-LINE QUASAR PMN J0948+0022 (2009, methodology): “The complete description of the general model used can be found in Ghisellini & Tavecchio (2009); here we briefly summarize the main parameters: • the source is assumed to be located at a distance Rdiss = 6.75 × 10 16 cm from a black hole of mass M = 1.5 × 108M⊙; • the source is assumed to be a…”
- Properties of flat-spectrum radio-loud Narrow-Line Seyfert 1 Galaxies (2014, background): “The size of the BLR gives also the luminosity of the accretion disk (RBLR ∝ L 1/2 disk, e.g. Ghisellini & Tavecchio 2009; see also Bentz et al. 2013), which in turn has been normalised to the Article number, page 9 of 35 Eddington value LEdd = 1.3× 10 38 ( M M⊙ ) [erg s−1].”
- TeV BL Lac objects at the dawn of the Fermi era (2009, background): “In BL Lacs, instead, the small cooling allows the electrons to be accelerated to very high energy, determining high frequencies for the synchrotron and IC emission components (see Ghisellini & Tavecchio 2008a, 2009 for a refined view).”
- PROBING THE INNER JET OF THE QUASAR PKS 1510−089 WITH MULTI-WAVEBAND MONITORING DURING STRONG GAMMA-RAY ACTIVITY (2010, background): “…was close to the base of the jet, electrons in the jet could have scattered the broad emission-line region or accretion-disk photons to γ-ray energies as the disturbance first became optically thin to photon-photon pair production (see, e.g., Ghisellini & Tavecchio 2009; Dermer et al. 2009).”
- The Fermi blazar sequence (2017, methodology): “This model is described in Ghisellini & Tavecchio (2009).”
- GeV BREAKS IN BLAZARS AS A RESULT OF GAMMA-RAY ABSORPTION WITHIN THE BROAD-LINE REGION (2010, background): “The observed spectral breaks are also too sharp and the change in the spectral indices are too large to be associated with the cooling or the Klein-Nishina effects (Ghisellini & Tavecchio 2009).”
- MAGIC DISCOVERY OF VERY HIGH ENERGY EMISSION FROM THE FSRQ PKS 1222+21 (2011, background): “This is due to the combination of two effects: the decreased efficiency of the IC scattering occuring in the Klein-Nishina (KN) regime (e.g. Ghisellini & Tavecchio 2009) and the absorption of γ-rays through pair production (Reimer 2007; Tavecchio & Mazin 2009; Liu & Bai 2006) 4.”