An optimization principle for computing stationary MHD equilibria with solar wind flow
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In this work we describe a numerical optimization method for computing stationary MHD-equilibria. The newly developed code is based on a nonlinearforce-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 β and Alfvén Mach number MA 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 β and MA 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.
Wiegelmann , T , Neukirch , T , Nickeler , D & Chifu , I 2020 , ' An optimization principle for computing stationary MHD equilibria with solar wind flow ' , Solar Physics , vol. 295 , no. 10 , 145 . https://doi.org/10.1007/s11207-020-01719-8
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DescriptionTW acknowledges financial support by DLR-grant 50 OC 1701 and DFG-grant WI 3211/5-1. TN acknowledges financial support by the UK’s Science and Technology Facilities Council (STFC) via Consolidated Grant ST/S000402/1. The Astronomical Institute of the Czech Academy of Sciences is supported by the project RVO:67985815. IC acknowledges funding by DFG-grant WI 3211/5-1.
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