Weak Alfvénic turbulence in relativistic plasmas. Part 2. current sheets and dissipation

Alfvén waves as excited in black hole accretion disks and neutron star magnetospheres are the building blocks of turbulence relativistic, magnetized plasmas. A large reservoir magnetic energy is available these systems, such that plasma can be heated significantly even weak regime. We perform high-resolution three-dimensional simulations counter-propagating waves, showing an $E_{B_{\perp }}(k_{\perp }) \propto k_{\perp }^{-2}$ spectrum develops a result cascade relativistic magnetohydrodynamics its infinitely (force-free) limit. The ubiquitously generates current sheets, which act locations where dissipates. show sheets form natural nonlinear interactions between waves. These owing to compression elongated eddies, driven by shear induced growing higher-order modes, undergo thinning process until they break-up into small-scale turbulent structures. explore formation both overlapping localized wave packet collisions. interaction induces fast efficiently mediates conversion dissipation electromagnetic astrophysical systems. Plasma energization through reconnection emerging during potentially explain X-ray emission coronae magnetospheres.