An optimization principle for the computation of MHD equilibria in the solar corona

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作者：
Wiegelmann, T. [1 ]
Neukirch, T. [2 ]
机构：
[1] Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
[2] School of Mathematics and Statistics, University of St. Andrews, St. Andrews, KY16 9SS, United Kingdom
来源：
Astronomy and Astrophysics | 1600年 / 457卷 / 03期
关键词：
Aims. We develop an optimization principle for computing stationary MHD equilibria. Methods. Our code for the self-consistent computation of the coronal magnetic fields and the coronal plasma uses non-force-free MHD equilibria. Previous versions of the code have been used to compute non-linear force-free coronal magnetic fields from photospheric measurements. The program uses photospheric vector magnetograms and coronal EUV images as input. We tested our reconstruction code with the help of a semi-analytic MHD-equilibrium. The quality of the reconstruction was judged by comparing the exact and reconstructed solution qualitatively by magnetic field-line plots and EUV-images and quantitatively by several different numerical criteria. Results. Our code is able to reconstruct the semi-analytic test equilibrium with high accuracy. The stationary MHD optimization code developed here has about the same accuracy as its predecessor; a non-linear force-free optimization code. The computing time for MHD-equilibria is; however; longer than for force-free magnetic fields. We also extended a well-known class of nonlinear force-free equilibria to the non-force-free regime for purposes of testing the code. Conclusions. We demonstrate that the code works in principle using tests with analytical equilibria; but it still needs to be applied to real data. © ESO 2006;
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Journal article (JA)
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页码：1053 / 1058
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