In the same paper, the section on "Turbulence and Reconnection in Relativistic Plasmas" is also very interesting. It talks about the turbulence in fast moving plasmas:
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Dissipation of turbulent motion leads to plasma heating, generation of magnetic field and, most importantly, acceleration of particles to super-thermal energies. Astrophysical turbulence provides a way for the macroscopic energy to be dissipated into kinetic energy of particle motion, which in turn produces a wide range of observable radiation.
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This includes: solar flares, solar wind heating, accretion disks around pre-main sequence stars and compact objects, various interstellar medium processes (proto-stellar clouds), supernova remnants, AGN jets and cluster galaxy processes.
For corona of magnetars, AGN and GRB jets:
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where energy density of magnetic field exceeds plasma energy density, including rest mass. What are the spectra and anisotropic properties of turbulence in this case? Virtually in all of these turbulence types the key questions are the same: what are the spectra and anisotropic properties of the fluctuating quantities on different scales, and what are the spectra of particles accelerated, presumably, by Fermi-type mechanism.
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All good research/investigation topics which I'm sure would help explain a lot more of the phenomena/observations surrounding these objects.
Good stuff.
Cheers