Computer Science – Numerical Analysis
Scientific paper
Nov 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983nascp.2280..23p&link_type=abstract
In JPL Solar Wind Five p 23-32 (SEE N84-13067 03-92)
Computer Science
Numerical Analysis
Convective Heat Transfer, Electrical Resistivity, Heating, Magnetic Fields, Solar Corona, Current Density, Magnetohydrodynamic Waves, Numerical Analysis, Pressure Effects, Tearing Modes (Plasmas), Viscosity
Scientific paper
The visible corona of the Sun appears to be heated by direct dissipation of magnetic fields. The magnetic fields in the visible corona are tied at both ends to the photosphere where the active convection continually rotates and shuffles the footpoints in a random pattern. The twisting and wrapping of flux tubes about each other produce magnetic neutral sheets in a state of dynamical nonequilibrium such that the current sheets become increasingly concentrated with the passage of time. Dissipation of the high current densities takes place regardless of the high electrical conductivity of the fluid. The convection on the feet of the lines of force at the surface of the Sun goes directly (within a matter of 10 to 20 hours) into heat in the corona. The rate of doing work seems adequate to supply the necessary 10 to the 7th power ergs/square cm. sec for the active corona.
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