A study of physical mechanisms for filament eruption and coronal mass ejection via numerical simulation

Details A study of physical mechanisms for filament eruption and coronal mass ejection via numerical simulation A study of physical mechanisms for filament eruption and coronal mass ejection via numerical simulation

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991stin...9318577w&link_type=abstract

Progress Report, 1 Jan. - Jun. 1991 Alabama Univ., Huntsville. Dept. of Mechanical Engineering and Center for Space Plasma and A

Physics

Magnetohydrodynamic Stability, Photosphere, Solar Corona, Solar Flares, Solar Magnetic Field, Stellar Mass Ejection, Gravitational Effects, Magnetohydrodynamics, Plasmas (Physics), Time Dependence

Scientific paper

It is well-known from both observation and theory that photospheric shear motion has played a key role in physical processes of the energy build-up and release for the solar flare. In order to further our understanding of the occurrence of solar flares it is necessary to investigate the triggering mechanism. One popular scenario for the onset of eruptive solar flares is that in response to photospheric shear motions the magnetic field evolves slowly through a series of magnetohydrodynamic-equilibria until a threshold is reached where magnetohydrodynamic (MHD) non-equilibrium sets in. Thus, a magnetic eruption occurs, causing the solar flare. To substantiate this claim we have employed our newly developed three-dimensional time-dependent MHD code with gravity to simulate the evolution of the coronal field. We use plasma beta = 0.1 to closely approximate the condition in the actual corona. Some preliminary results are presented.

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