| タイトル | A Method for Localizing Energy Dissipation in Blazars Using Fermi Variability |
| 本文（外部サイト） | http://hdl.handle.net/2060/20130011775 |
| 著者（英） | Kazanas, Demosthenes; Perlman, Eric S.; Dotson, Amanda; Georganopoulos, Markos |
| 著者所属（英） | NASA Goddard Space Flight Center |
| 発行日 | 2013-01-03 |
| 言語 | eng |
| 内容記述 | The distance of the Fermi-detected blazar gamma-ray emission site from the supermassive black hole is a matter of active debate. Here we present a method for testing if the GeV emission of powerful blazars is produced within the sub-pc scale broad line region (BLR) or farther out in the pc-scale molecular torus (MT) environment. If the GeV emission takes place within the BLR, the inverse Compton (IC) scattering of the BLR ultraviolet (UV) seed photons that produces the gamma-rays takes place at the onset of the Klein-Nishina regime. This causes the electron cooling time to become practically energy independent and the variation of the gamma-ray emission to be almost achromatic. If on the other hand the -ray emission is produced farther out in the pc-scale MT, the IC scattering of the infrared (IR) MT seed photons that produces the gamma-rays takes place in the Thomson regime, resulting to energy-dependent electron cooling times, manifested as faster cooling times for higher Fermi energies. We demonstrate these characteristics and discuss the applicability and limitations of our method. |
| NASA分類 | Astronomy |
| レポートNO | GSFC-E-DAA-TN7192 |
| 権利 | Copyright, Distribution as joint owner in the copyright |
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