Other
Scientific paper
Apr 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...255..730s&link_type=abstract
Astrophysical Journal, Part 1, vol. 255, Apr. 15, 1982, p. 730-742.
Other
109
Coronal Holes, Magnetohydrodynamic Flow, Plasma Dynamics, Solar Corona, Solar Magnetic Field, Beta Factor, Isothermal Flow, Lines Of Force, Steady State, Stellar Models
Scientific paper
The formation of the steady coronal structure which consists of coronal streamers and holes is seen in terms of a model employing numerical solutions of time-dependent, dissipationless, magnetohydrodynamic equations of motion applicable to the meridional plane. A coronal streamer consists of closed magnetic field lines near the solar surface with overlying and adjacent open field lines, and the atmosphere, which is stationary in the closed region, flows outward in the open region, or coronal hole. The steady coronal structure is obtained by starting the numerical calculation with a state comprising a polytropic, hydrodynamical solution to the steady-state radial equation of motion coupled with a dipole magnetic field. Global coronal configurations are calculated for values of the plasma beta which vary from 0.1 to 100. It is found that the height and lateral extension of the closed region are only weakly dependent on the data.
Steinolfson Richard S.
Suess Steve T.
Wu Shi Tsan
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