Application of the MHD energy principle to magnetostatic atmospheres

Details Application of the MHD energy principle to magnetostatic atmospheres Application of the MHD energy principle to magnetostatic atmospheres

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985gapfd..32..317z&link_type=abstract

Geophysical and Astrophysical Fluid Dynamics (ISSN 0309-1929), vol. 32, no. 3-4, 1985, p. 317-331. Previously announced in STAR

Physics

15

Boundary Layer Stability, Chromosphere, Fluid Boundaries, Interface Stability, Magnetohydrodynamic Stability, Plasma Dynamics, Solar Corona, Perturbation Theory, Solar Atmosphere, Solar Magnetic Field, Solar Physics

Scientific paper

The author applies the MHD energy principle to the stability of a magnetized atmosphere which is bounded below by much denser fluid, as is the solar corona. The author treats the two fluids as ideal; the approximation which is consistent with the energy principle, and uses the dynamical conditions that must hold at a fluid-fluid interface to show that if vertical displacements of the lower boundary are permitted, then the lower atmosphere must be perturbed as well. However, displacements which do not perturb the coronal boundary can be properly treated as isolated perturbations of the corona alone.

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