"Theory and simulations of solar system plasmas" aims to highlight results from microscopic to global scales, achieved by theoretical investigations and numerical simulations of the plasma dynamics in the solar system. The theoretical approach must allow evidencing the universality of the phenomena being considered, whatever the region is where their role is studied; at the Sun, in the solar corona, in the interplanetary space or in planetary magnetospheres. All possible theoretical issues concerning plasma dynamics are welcome, especially those using numerical models and simulations, since these tools are mandatory whenever analytical treatments fail, in particular when complex nonlinear phenomena are at work.

In this view we encourage all contributions addressing the problem of complexity, cross-scale coupling and the different approaches to turbulence, questions that can be linked through theory and simulations now to the results obtained by multi-point space experiments. Closely related appears the issue of driven reconnection: waves, turbulence or structures are indeed able to break the frozen in hypothesis, either directly, by the small scales they provide, or indirectly, by forcing stable layers toward an unstable state.