"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, the 2010 issue will emphasize the questions concerning the interface between fluid and kinetic descriptions. Do the kinetic models largely depart from the fluid ones (typically MHD) when investigating 'large scale' phenomena such as solar wind expansion or KH non linear evolution? Are there free parameters that can be plugged in fluid models to correctly mimic the kinetic ones? How can both kinds of models help in understanding the great well-known cross-scale phenomena such as collisionless shocks and reconnection?