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The dynamics of a dissipative Poynting dominated flow subject to a radiationdrag due to Compton scattering of ambient photons by relativistic electronsaccelerated in reconnecting current sheets is studied. It is found that theefficiency at which magnetic energy is converted to radiation is limited to amaximum value of $\epsilon_c=3l_{dis}\,\sigma_0/4(\sigma_0+1)$, where$\sigma_0$ is the initial magnetization of the flow and $l_{dis}\le1$ thefraction of initial Poynting flux that can dissipate. The asymptotic Lorentzfactor 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 caseswhere the cooling time is shorter than the local dissipation time. A somewhatsmaller radiative efficiency is expected if radiative losses are dominated bysynchrotron and SSC emissions. It is suggested that under certain conditionsmagnetic field dissipation may occur in two distinct phases: On small scales,asymmetric magnetic fields that are advected into the polar region and draggedout by the outflow dissipate to a more stable configuration. The dissipatedenergy is released predominantly as gamma rays. On much larger scales, theoutflow encounters a flat density profile medium and re-collimates. This leadsto further dissipation and wobbling of the jet head by the kink instability, asfound recently in 3D MHD simulations. Within the framework of a model proposedrecently to explain the dichotomy of radio loud AGN, this scenario can accountfor the unification of gamma-ray blazars with FRI and FRII radio sources.

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