It is a challenge to construct models of realistic plasma phenomena,
but it is a requirement to validate model results against observations.
For the solar corona, we see hot loops that emit extreme UV light with
Doppler shifts. In the case of magnetic reconnection, non-thermal
electrons are produced and are later thermalized, like in the
magnetospheres of planets or during flares on the Sun. We investigate
in how far these processes are interconnected. The physical driver for
reconnection in the solar corona is the convection at its surface. It
is necessary to check the robustness of the numerical results. Also we
know that space plasmas are magnetized at different levels. This fact
gives rise to the formation of an electromotive force that may cause
dynamo effects throughout the heliosphere, which we can measure, too.
We find that this often disregarded force is effective e.g. during
inter-planetary coronal mass ejections and dipolarization fronts.