Physics
Scientific paper
Feb 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...83...63r&link_type=abstract
(Lindau Workshop on the Source Region of the Solar Wind, 9th, Lindau, West Germany, Nov. 1981.) Solar Physics, vol. 83, Feb. 198
Physics
25
Coronal Holes, Magnetic Effects, Magnetohydrodynamic Flow, Plasma Interactions, Solar Magnetic Field, Current Density, Flow Velocity, Gravitational Effects, Iterative Solution, Plasma Dynamics, Temperature Distribution
Scientific paper
Magnetic fields are thought to play a crucial role in determining the dynamics and energetics of coronal hole flows. In this paper the possibility that the large scale structure of the magnetic field and plasma within a coronal hole may be determined from the effects of plasma-magnetic field interactions is investigated. The overall state is then governed by a complex balance of inertial, pressure gravitational and magnetic forces. Integration of the highly nonlinear system of differential equations, which describe the plasma-magnetic field coupling, is made possible by employing a numerical iterative technique developed by Pneuman and Kopp (1971). The method of solution is modified and extended to describe thermally conductive plasma flow in coronal holes. The features of a typical converged solution, representing the distribution of velocity, temperature, density and magnetic field strength within a coronal hole, are considered.
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