Interactions Between Radio Galaxies and Cluster Shocks – 1: Jet Axes Aligned with Shock Normals. (arXiv:1904.05943v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Nolting_C/0/1/0/all/0/1">Chris Nolting</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_T/0/1/0/all/0/1">T. W. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+ONeill_B/0/1/0/all/0/1">Brian O'Neill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mendygral_P/0/1/0/all/0/1">P. J. Mendygral</a>
We report from a study utilizing 3D MHD simulations, including cosmic-ray
electrons, of the interactions between radio galaxies (RGs) and dynamically
active ICMs. Here we consider interactions involving plane ICM shocks having
Mach numbers 2–4 and their normals aligned with steady, active bipolar RG jets
penetrating uniform, stationary ICMs. Shock impact disrupts the pre-formed RG
jet cocoons into ring vortex structures. Sufficiently strong post-shock winds
can stop and even reverse the upwind jet, and strip jets to virtually “naked”
states, leaving them without a surrounding cocoon. Strong shock-induced
vorticity can also disrupt the downwind jet, so that the ring vortex remnant of
the cocoons appears ahead of that jet’s visible terminus. Magnetic field
amplification in the ring vortex can significantly enhance its synchrotron
emissions well after the vortex becomes isolated from the RG and its fresh CRe
supply. We examine these dynamics and their observable consequences in detail.
We report from a study utilizing 3D MHD simulations, including cosmic-ray
electrons, of the interactions between radio galaxies (RGs) and dynamically
active ICMs. Here we consider interactions involving plane ICM shocks having
Mach numbers 2–4 and their normals aligned with steady, active bipolar RG jets
penetrating uniform, stationary ICMs. Shock impact disrupts the pre-formed RG
jet cocoons into ring vortex structures. Sufficiently strong post-shock winds
can stop and even reverse the upwind jet, and strip jets to virtually “naked”
states, leaving them without a surrounding cocoon. Strong shock-induced
vorticity can also disrupt the downwind jet, so that the ring vortex remnant of
the cocoons appears ahead of that jet’s visible terminus. Magnetic field
amplification in the ring vortex can significantly enhance its synchrotron
emissions well after the vortex becomes isolated from the RG and its fresh CRe
supply. We examine these dynamics and their observable consequences in detail.
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