Local potential analysis of MHD instability

Details Local potential analysis of MHD instability Local potential analysis of MHD instability

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ap%26ss.109..131s&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 109, no. 1, Feb. 1985, p. 131-143.

Statistics

Computation

Computational Astrophysics, Interstellar Gas, Magnetohydrodynamic Stability, Stellar Atmospheres, Compressible Fluids, Interstellar Masers, Variational Principles

Scientific paper

The use of the local potential method for studying instabilities of MHD fluids is examined. The mathematical method is similar to that developed by the authors for studying the time-dependent radiative transfer problem and the radiative stability of interstellar masers. The scheme is based on the universal evolution criterion proposed by Glansdorff and Prigogine (1964) as demonstrated by Hays (1965) for the heat equation and Schechter and Himmelblau (1965) for the Benard problem in hydrodynamics. The scheme for securing stability criteria is demonstrated for two particular cases.

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