Speaker
Description
Turbulent flows are believed to be present in the solar corona, especially in connection with solar flares and coronal mass ejections. They are supposed to be very effective processes in energy transportation and can contribute to the heating of the solar corona. We study turbulence in reconnection outflows associated with flares and CMEs. We simulate the generation and evolution of the turbulent plasma flow and investigate its energies and formed plasma velocity and magnetic field structures. For the numerical simulations, we adopt a 3D magnetohydrodynamic (MHD) model, in which we solve a full set of the 3D time-dependent resistive and compressible MHD equations using the Lare3d numerical code. We numerically study turbulence in the plasma flow in the model with the plasma parameters that could simulate processes in the magnetic reconnection outflows in solar flares. Starting from a non-turbulent plasma flow in the energetically closed system, we studied the evolution of the kinetic, internal and magnetic energies during the turbulence generation. We found that most of the kinetic energy was transformed into plasma heating (about 95 %) and only a small part of the magnetic energy (about 5 %). The turbulence in the system evolved to the saturation stage with the power-law index of the kinetic density spectrum −5/3. Magnetic energy was also saturated due to its dissipation and reconnection in small and complex magnetic field structures. We show examples of the structures formed in studied turbulent flow: velocity vortices, magnetic field cocoons and plasmoids.
