Energy dynamics in stressed magnetic fields - The filamentation and flare instabilities

Details Energy dynamics in stressed magnetic fields - The filamentation and flare instabilities Energy dynamics in stressed magnetic fields - The filamentation and flare instabilities

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...268..860v&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 268, May 15, 1983, p. 860-864. NASA-NSF-supported research.

Astronomy and Astrophysics

Astrophysics

18

Magnetohydrodynamic Stability, Solar Flares, Solar Magnetic Field, Solar Prominences, Finite Difference Theory, Tearing Modes (Plasmas), Thermal Stability

Scientific paper

The thermal and tearing instabilities are believed to be the two primary temperature modification mechanisms in sheared astrophysical magnetic fields. The former gives rise to the formation of cool filaments and the latter to the release of magnetic energy. It has long been known that these processes are interrelated, most conspicuously in the case of the solar corona where prominences often precede flares within the same magnetic structure. It is also clear, from first principles, that the energy transport underlying the thermal instability should have a strong effect on the resistivity which facilitates magnetic tearing, and that the energy release of the latter should affect the temperature drop of the former. This paper describes some results of the first calculations which attempt to unify the dynamic treatment of these two coexisting instabilities. Growth rates as a function of resistivity, and examples of the primary mode structures are provided, along with a discussion of some critical aspects of the interaction of these two astrophysical energy flux mechanisms.

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