Wednesday

Magnetic reconnection in the solar corona is an essentially kinetic process since the plasma is practically collisionless. It can only remotely be diagnosed, mostly by indirect observational methods. The best plasma diagnostics of its plasma and magnetic field properties can be provided by radio-astronomical observations of the Sun. In order to deduce the relevant information about plasma and field parameters from radio-signals information about the formation of velocity space distribution of the electrons accelerated by magnetic reconnection is required.
3D PIC-code- simulations of kinetic magnetic reconnection for solar coronal field and plasma conditions have been carried out which allow to derive the evolution of electron velocity space distribution functions due to kinetic reconnection. The arising sources of free energy for plasma and electromagnetic wave generation have been analyzed. For typical distribution functions the consequent plasma instabilities have been found and the properties of the waves were calculated. Out of them predictions for observables can be derived. The most recent results are reviewed here.