Constraints on Blazar Jet Conditions During Gamma-Ray Flaring from Radiative Transfer Modeling

¹ Department of Astronomy, University of Michigan, 817 Dennison Bldg., Ann Arbor MI 48109-1042 USA
² Cahill Center for Astronomy & Astrophysics, California Institute of Technology 1200 E. California Blvd., Pasadena CA 91125 USA

^a e-mail: mfa@umich.edu

Published online: 9 December 2013

Abstract

As part of a program to investigate jet flow conditions during GeV gamma-ray flares detected by Fermi, we are using UMRAO multi-frequency, centimeter-band total flux density and linear polarization monitoring observations to constrain radiative transfer models incorporating propagating shocks orientated at an arbitrary angle to the flow direction. We describe the characteristics of the model, illustrate how the data are used to constrain the models, and present results for three program sources with diverse characteristics: PKS 0420-01, OJ 287, and 1156+295. The modeling of the observed spectral behavior yields information on the sense, strength and orientation of the shocks producing the radio-band flaring; on the energy distribution of the radiating particles; and on the observer’s viewing angle with respect to the jet independent of VLBI data. We present evidence that, while a random component dominates the jet magnetic field, a distinguishing feature of those radio events with an associated γ-ray flare is the presence of a weak but non-negligible ordered magnetic field component along the jet axis.