Global coronal and heliospheric magnetic field modelling for Solar Orbiter

Computing the solar coronal magnetic field and plasma
environment is an important research topic on it's own right
and also important for space missions like Solar Orbiter to
guide the analysis of remote sensing and in-situ instruments.
In the inner solar corona plasma forces can be neglected and
the field is modelled under the assumption of a vanishing
Lorentz-force. Further outwards (above about two solar radii)
plasma forces and the solar wind flow has to be considered.
Finally in the heliosphere one has to consider that the Sun
is rotating and the well known Parker-spiral forms.
We have developed codes based on optimization principles
to solve nonlinear force-free, magneto-hydro-static and
stationary MHD-equilibria. In the present work we want to
extend these methods by taking the solar rotation into account.