Numerical simulation of a magnetic reconnection in the solar corona

Details Numerical simulation of a magnetic reconnection in the solar corona Numerical simulation of a magnetic reconnection in the solar corona

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990stin...9215952w&link_type=abstract

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Magnetic Field Reconnection, Solar Corona, Solar Magnetic Field, Space Plasmas, Magnetic Field Configurations, Magnetohydrodynamics, Mathematical Models, Stellar Mass Ejection

Scientific paper

In this paper, a kind of magnetic reconnection process caused by the local heating in the closed magnetic field region over the equator in the solar corona is discussed. At first, we use a method in combination with analytical and numerical methods to obtain a coronal magnetic configuration with an X-type neutral point. Furthermore we solve numerically the magnetohydrodynamic equations by using the full-implicit continuous Eulerian scheme in spherical coordinates. The results of numerical simulation show that three different processes of magnetic reconnection exist. On the other hand, the upward plasma velocity is small when the effect of the solar gravitational field is considered. Hence, we suggest that the magnetic reconnection caused by the pure resistivity tearing mode may be unimportant for the coronal mass ejections.

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