Physics – Fluid Dynamics
Scientific paper
Dec 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982gapfd..22..195p&link_type=abstract
Geophysical and Astrophysical Fluid Dynamics, vol. 22, no. 3-4, 1982, p. 195-218.
Physics
Fluid Dynamics
41
Conducting Fluids, Magnetic Field Configurations, Magnetic Flux, Magnetohydrodynamics, Nonequilibrium Plasmas, Solar Magnetic Field, Plasma Dynamics, Solar Prominences, Stellar Atmospheres, Velocity Distribution
Scientific paper
The dynamical conditions that exist when long straight parallel twisted flux tubes in a highly conducting fluid are packed together in a broad array are treated. It is shown that in general there is no hydrostatic equilibrium. In place of equilibrium, there is a dynamical nonequilibrium, which leads to neutral point reconnection and progressive coalescence of neighboring tubes (with the same sense of twisting); this in turn forms tubes of large diameter and reduced twist. The magnetic energy in the twisting of each tube declines toward zero, being dissipated into small-scale motions of the fluid and thence into heat. Referring to the sun, it is pointed out that the twisting and mutual wrapping is converted directly into fluid motion and heat by the dynamical nonequilibrium, so that the work done by the convection of the footpoints goes directly into heating the corona above.
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