Three Dimensional Numerical Study of Solar Coronal Magnetic Field Based on the Magnetograph Observations

Details Three Dimensional Numerical Study of Solar Coronal Magnetic Field Based on the Magnetograph Observations Three Dimensional Numerical Study of Solar Coronal Magnetic Field Based on the Magnetograph Observations

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aps..dppyp1021k&link_type=abstract

American Physical Society, 42nd Annual Meeting of the APS Division of Plasma Physics combined with the 10th International Congre

Physics

Plasma Physics

Scientific paper

Magnetohydrodynamic (MHD) properties of active regions in solar corona is investigated by combining the numerical analysis technique and the vector magnetograph observations. First, we numerically construct the potential magnetic field of several major active regions, and compare them with the tangential component of the magnetic field observed by Solar Flare Telescope in National Astronomical Observatory of Japan. As a result, we found that the magnetic free energy, which is formed by the the gap between the observed field and the potential field, as well as the current helicity, which is produced by the electric current and the magnetic field across the photosphere, is reduced in some big flare events. It suggests that the solar flares are processes to reduce the magnetic helicity contained in the coronal magnetic field. Secondly, we develop the numerical model to construct the three dimensional (3D) nonlinear equilibria in active regions using the vector magnetic field observed by magnetograph. Furthermore, the MHD stability of the practical solar corona will be discussed based on the numerical calculations using the observed data.

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