Physics
Scientific paper
May 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981soph...71..141y&link_type=abstract
Solar Physics, vol. 71, May 1981, p. 141-149.
Physics
15
Coronal Loops, Solar Corona, Solar Magnetic Field, Solar Wind, Buoyancy, Magnetohydrodynamic Flow, Mass Flow, Plasma Density, Pressure Gradients, Solar Gravitation, Stellar Mass Ejection, Surges
Scientific paper
The heliocentrifugal motion of coronal loop transients is likely driven largely by the buoyant force exerted by the ambient medium. In the outer corona where the solar wind is well formed, the buoyant force results mainly from the rapid outward decrease in the ambient pressure of the solar wind. The contribution from magnetic buoyancy is not so significant as in the vicinity of the solar surface. Therefore, the pertinent features of the loop transients in the outer corona are basically gasdynamical. As a conspicuous part of coronal expansion, the motion of the compressible masses in the transient loops is largely controlled by thermal forces. The translational motion of heliocentrifugal expansion is driven by the hydrodynamic buoyant force, and the lateral motion of peripheral expansion is driven by the pressure difference between the dense plasma of the ejecta and the tenuous plasma of the ambient medium.
Dryer Murray
Yen T.
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