Dynamics and energetics of the solar corona

Details Dynamics and energetics of the solar corona Dynamics and energetics of the solar corona

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992sri..reptq....s&link_type=abstract

Final Technical Report, Sep. 1989 - Aug. 1992 Southwest Research Inst., San Antonio, TX. Instrumentation and Space Research Div.

Computer Science

Numerical Analysis

Interplanetary Medium, Magnetohydrodynamics, Magnetoplasmadynamics, Numerical Analysis, Plasma Physics, Solar Corona, Stellar Mass Ejection, Magnetic Flux, Photosphere, Solar Magnetic Field, Time Dependence

Scientific paper

The primary objective of this research program is to improve our understanding of the dynamics and energetics of the solar corona both in the quiescent dynamic equilibrium state when coronal structure is dominated by the equatorial streamer belt and in the eruptive state when coronal plasma is ejected into the interplanetary medium. Numerical solutions of the time-dependent magnetohydrodynamic (MHD) equations and comparisons of the computed results with observations form the core of the approach to achieving this objective. Some of the specific topics that have been studied are: (1) quiescent coronal streamers in an atmosphere dominated by a dipole magnetic field at large radii, (2) the formation of coronal mass ejections (CMEs) in quiescent streamers due to the emergence of new magnetic flux and due to photospheric shear motion, (3) MHD shock formation near the leading edge of CMEs, (4) coronal magnetic arcade eruption as a result of applied photospheric shear motion, and (5) the three-dimensional structure of CMEs.

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