http://arxiv.org/abs/2010.02945
In this work we describe a numerical optimization method for computing stationary MHD-equilibria. The newly developed code is based on a nonlinear force-free optimization principle. We apply our code to model the solar corona using synoptic vector magnetograms as boundary condition. Below about two solar radii the plasma $\beta$ and Alfv\’en Mach number $M_A$ are small and the magnetic field configuration of stationary MHD is basically identical to a nonlinear force-free field, whereas higher up in the corona (where $\beta$ and $M_A$ are above unity) plasma and flow effects become important and stationary MHD and force-free configuration deviate significantly. The new method allows the reconstruction of the coronal magnetic field further outwards than with potential field, nonlinear force-free or magneto-static models. This way the model might help to provide the magnetic connectivity for joint observations of remote sensing and in-situ instruments on Solar Orbiter and Parker Solar Probe.
T. Wiegelmann, T. Neukirch, D. Nickeler, et. al.
Thu, 8 Oct 20
48/54
Comments: 18 pages, 6 figures, 2 tables, Solar Physics, accepted
You must be logged in to post a comment.