2008/10/06 by C. D. Dermer, Charles D. Dermer, Dermer, Charles D. +4
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics (astro-ph) #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.48550/arxiv.0810.1055
9 pages, 2 figures. prc. "Blazar variability across the electromagnetic spectrum", Palaiseau, France. Ed: Berrie Giebels
arxiv created 2008/10/06 · openalex publication_date 2008/10/06 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Kinematical and luminosity relations for black-hole jet sources are reviewed. If the TeV flares observed from PKS 2155-304 in 2006 July are assumed to originate from a black hole with mass ≈ 108 M8 M_\odot, then the ∼ 5 minute variability timescale is consistent with the light-travel time across the Schwarzschild radius of the black hole if M8∼ 1. The absolute jet power in a synchrotron/SSC model exceeds, however, the Eddington luminosity for a black hole with M8∼ 1 unless the jet is highly efficient. The maximum Blandford-Znajek power is ∼ 1046M8 ergs s-1 if the magnetic-field energy density threading the horizon is equated with the luminous energy density in the vicinity of the black hole. An external Compton component can relax power requirements, so a black hole with mass ∼ 108 M_\odot could explain the observed flaring behavior. For the Swift and HESS data taken in 2006 July, relativistic outflows with bulk Lorentz factor Γ\gtrsim 30 satisfy γ-γ attenuation limits. If this system harbors a binary black hole, then the accretion disk from a more massive, ∼ 109 M_\odot black-hole primary would make an additional external radiation component. Dual thermal accretion disk signatures would confirm this scenario.