1999/10/29 by K. S. Cheng, J. H. Fan, Cheng, K. S. +4
Engineering · Physics and Astronomy · #Astrophysics (astro-ph) #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #Gyrotron and Vacuum Electronics Research #Particle Accelerators and Free-Electron Lasers #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9910543
14 pages, 3 tables, A&A accepted
arxiv created 1999/10/29 · openalex publication_date 1999/10/29 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In this paper, a method is proposed to determine the basic properties of γ-ray loud blazars, among them the central black hole mass, M, the Doppler factor, δ, the propagation angle of the γ-rays with respect to the symmetric axis of a two-temperature accretion disk, Φ, and the distance (i.e. the height above the accretion disk), d at which the γ-rays are created, for seven γ-ray loud blazars with available GeV variability timescales and in which the absorption effect of a γ-ray and the beaming effect have been taken into account. Our results indicate that, if we take the intrinsic γ-ray luminosity to be λ times the Eddington luminosity, Lγin = λLEdd., the masses of the blazars are in the range of (4 ∼ 131)× 107M\odot, the Doppler factors (δ) lie in the range of 0.57 to 5.33 the angle (Φ) is in the range of 13∘ to 43∘ and the distance (d) is in the range of 26Rg to 411Rg. Our model results are independent of γ-ray emission mechanisms but they do depend on the X-ray emission mechanism of the accretion disk.