The Parker model for coronal heating is investigated through a high resolution simulation. An inertial range is resolved where fluctuating magnetic energy E_M (k_perp) \propto k_\perp^{ -2.7} exceeds kinetic energy E_K (k_\perp) \propto k_\perp^{ -0.6}. Increments scale as \delta b_\ell \simeq \ell^{ -0.85} and \delta u_\ell \simeq \ell^{ +0.2} with velocity increasing at small scales, indicating that magnetic reconnection plays a prime role in this turbulent system. We show that spectral energy transport is akin to standard magnetohydrodynamic (MHD) turbulence even for a system of reconnecting current sheets sustained by the boundary. In this new MHD turbulent cascade, kinetic energy flows are negligible while cross-field flows are enhanced, and through a series of "reflections" between the two fields, cascade more than half of the total spectral energy flow.
Categories: astro-ph.SR astro-ph.EP physics.plasm-ph