The stability of coronal and prominence magnetic fields

Details The stability of coronal and prominence magnetic fields The stability of coronal and prominence magnetic fields

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442..457h&link_type=abstract

In NASA. Goddard Space Flight Center Coronal and Prominence Plasmas p 457-460 (SEE N87-20871 13-92)

Other

Magnetic Fields, Magnetohydrodynamic Stability, Mathematical Models, Prominences, Solar Corona, Ballooning Modes, Boundary Value Problems, Linear Equations, Photosphere

Scientific paper

The magnetic fields in prominences and active regions (coronal arcades) may be susceptible to a variety of instabilities. Ideal MHD instabilities are the fastest growing and criteria for checking stability are complicated by the line tying effect of the dense photosphere. The significance of the localised instabilities is not yet fully understood. The nonlinear coupling of these modes may give rise to an explosive instability, with the modes coupling to longer wavelengths, (Mondt and Weiland, 1985). On the other hand, if the modes saturate early, then the main effect of the instability may be an enhancement of transport coefficients. Nonetheless, the author gives an equation which provides a simple test for the stability of cylindrical magnetic fields.

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