Physics
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..108..347s&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 108, no. 2, 1987, p. 347-382. USAF-supported research.
Physics
2
Cylindrical Plasmas, Magnetohydrodynamic Stability, Solar Flares, Solar Gravitation, Stellar Mass Ejection, Linear Equations, Magnetohydrodynamic Flow
Scientific paper
The linear MHD instability of a cylindrical plasma is used to investigate the origin of solar mass ejections, and the dispersion relation is solved numerically. The initial plasma-flow velocity is found to have a significant effect on the instability criteria and growth rate, and the instability growth-rate is shown to be larger in cases where plasma flow exists, relative to the static case. Results suggest that the plasma column may break into small pieces. Assuming a thin-tube approximation, gravity is found to have little effect on the instability of quasi-horizontal ejection, but to have considerable effect on the vertical ejection. In considering the gravitational force, an exact analytical solution is found for the vertical case, while asymptotic solutions are given for the horizontal and oblique cases.
Dryer Murray
Song Mu-Tao
Wu Shi Tsan
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