Show simple item record

dc.contributor.authorDotson, Amanda
dc.contributor.authorGeorganopoulos, Markos
dc.contributor.authorKazanas, Demosthenes
dc.contributor.authorPerlman, Eric S.
dc.date.accessioned2013-06-27T17:52:42Z
dc.date.available2013-06-27T17:52:42Z
dc.date.issued2012-10-10
dc.identifier.citationDotson, Amanda; Georganopoulos, Markos; Kazanas, Demosthenes; & Perlman, Eric. S. (2012). A method for localizing energy dissipation in blazars using Fermi variability. The Astrophysical Journal Letters, 758(1), L15.en_US
dc.identifier.urihttp://iopscience.iop.org/2041-8205/758/1/L15
dc.identifier.urihttp://hdl.handle.net/11141/61
dc.description.abstractThe distance of a Fermi-detected blazar γ-ray emission site from a 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 subparsec-scale broad-line region (BLR) or farther out in the parsec-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 γ-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 γ-ray emission to be almost achromatic. If, on the other hand, the γ-ray emission is produced farther out in the parsec-scale MT, the IC scattering of the infrared (IR) MT seed photons that produces the γ-rays takes place in the Thomson regime, resulting in 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.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is available in accordance with the publisher's policy. It may be subject to U.S. copyright law.en_US
dc.rights.urihttp://aas.org/publications/aas-copyright-policyen_US
dc.titleA method for localizing energy dissipation in blazars using Fermi variabilityen_US
dc.typeArticleen_US
dc.identifier.doi10.1088/2041-8205/758/1/L15


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record