Physics
Scientific paper
Mar 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976soph...47..193n&link_type=abstract
(NASA, IAU, IUGG, and International Council of Scientific Unions, Workshop on Flare Build-up Study, Falmouth, Mass., Sept. 8-11,
Physics
14
Energy Storage, Kinetic Energy, Magnetohydrodynamic Flow, Solar Atmosphere, Solar Magnetic Field, Chromosphere, Dynamic Response, Flow Velocity, Magnetic Flux, Self Consistent Fields, Solar Prominences, Velocity Distribution
Scientific paper
The dynamic response of the solar atmosphere is examined with the use of self-consistent numerical solutions to the complete set of nonlinear two-dimensional hydromagnetic equations. Of particular interest are the magnetic-energy buildup and the velocity field established by emerging flux at the base of an existing magnetic loop structure in a stationary atmosphere. For a plasma with a relatively low beta (0.03), the magnetic-energy buildup is approximately twice that of the kinetic energy, while the buildup in magnetic energy first exceeds but is eventually overtaken by the kinetic energy for a plasma with an intermediate beta (3). The increased magnetic flux causes the plasma to flow upward near the loop center and downward near the loop edges for the low-beta plasma. The plasma eventually flows downward throughout the lower portion of the loop carrying the magnetic field with it for the intermediate beta plasma. It is hypothesized that this latter case, and possibly the other case as well, may provide a reasonable simulation of the disappearance of prominences by flowing down into the chromosphere (a form of disparition brusque).
Nakagawa Yasuhiro
Steinolfson Richard S.
Wu Shi Tsan
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