Towards a rigorous model for multifluid expansions of stellar coronae : application to the solar wind

The existing standard MHD stellar wind models are extended in two new models. For the first, the treatment of the thermal properties of electrons and protrons is completed by numerical integration of two temperature equations describing for both constituents the components parallel and perpendicular to the magnetic field. For the second, the motion of electrons and protons are separated by consideration of two corresponding momentum equations including mutual friction terms and the electric polarisation field due to the different scale heights and expansion characteristics of the two species.