The effect of Compton drag on the dynamics of dissipative Poynting dominated flows: Implications for the unification of radio loud AGN

TL;DR

This paper investigates how Compton drag influences the dynamics and radiation efficiency of Poynting dominated flows, with implications for understanding the unification of radio loud AGN and their jet behaviors.

Contribution

It introduces a model for the effects of Compton drag on dissipative Poynting flows, linking magnetic dissipation, radiation efficiency, and jet dynamics in AGN.

Findings

Maximum radiative efficiency depends on initial magnetization and dissipation fraction.

Asymptotic Lorentz factor increases with initial conditions and dissipation.

Magnetic dissipation may occur in two phases, affecting gamma-ray emission and jet stability.

Abstract

The dynamics of a dissipative Poynting dominated flow subject to a radiation drag due to Compton scattering of ambient photons by relativistic electrons accelerated in reconnecting current sheets is studied. It is found that the efficiency at which magnetic energy is converted to radiation is limited to a maximum value of $\epsilon_c=3l_{dis}\,\sigma_0/4(\sigma_0+1)$, where $\sigma_0$ is the initial magnetization of the flow and $l_{dis}\le1$ the fraction of initial Poynting flux that can dissipate. The asymptotic Lorentz factor satisfies $\Gamma_\infty\ge\Gamma_0(1+l_{dis}\,\sigma_0/4)$, where $\Gamma_0$ is the initial Lorentz factor. This limit is approached in cases where the cooling time is shorter than the local dissipation time. A somewhat smaller radiative efficiency is expected if radiative losses are dominated by synchrotron and SSC emissions. It is suggested that under certain conditions magnetic field dissipation may occur in two distinct phases: On small scales, asymmetric magnetic fields that are advected into the polar region and dragged out by the outflow dissipate to a more stable configuration. The dissipated energy is released predominantly as gamma rays. On much larger scales, the outflow encounters a flat density profile medium and re-collimates. This leads to further dissipation and wobbling of the jet head by the kink instability, as found recently in 3D MHD simulations. Within the framework of a model proposed recently to explain the dichotomy of radio loud AGN, this scenario can account for the unification of gamma-ray blazars with FRI and FRII radio sources.