Theoretical Study Of The Effects Of Magnetic Field Geometry On The
  High-Energy Emission Of Blazars
  The knowledge of the structure of the magnetic field inside a blazar jet, as
deduced from polarization observations at radio to optical wavelengths, is
closely related to the formation and propagation of relativistic jets that
result from accretion onto supermassive black holes. However, a largely
unexplored aspect of the theoretical understanding of radiation transfer
physics in blazar jets has been the magnetic field geometry as revealed by the
polarized emission and the connection between the variability in polarization
and flux across the spectrum. Here, we explore the effects of various magnetic
geometries that can exist inside a blazar jet: parallel, oblique, toroidal, and
tangled. We investigate the effects of changing the orientation of the magnetic
field, according to the above-mentioned geometries, on the resulting
high-energy spectral energy distributions (SEDs) and spectral variability
patterns (SVPs) of a typical blazar. We use the MUlti-ZOne Radiation Feedback
(MUZORF) model of Joshi et al. (2014) to carry out this study and to relate the
geometry of the field to the observed SEDs at X-ray and gamma-ray energies.
  One of the goals of the study is to understand the relationship between
synchrotron and inverse Compton peaks in blazar SEDs and the reason for the
appearance of gamma-ray "orphan flares" observed in some blazars. This can be
associated with the directionality of the magnetic field, which creates a
difference in the radiation field as seen by an observer versus that seen by
the electrons in the emission region.
