An Optimization Principle for Computing Stationary MHD Equilibria With Solar Wind Flow

Abstract

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 Alfvén 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.

arXiv comment18 pages, 6 figures, 2 tables, Solar Physics, accepted

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Cited by in corpus (2)

• Global Coronal Equilibria with Solar Wind Outflow
• Evaluation of Coronal and Interplanetary Magnetic Field Extrapolation Using PSP Solar Wind Observation