Convective instability of thin flux tubes

Details Convective instability of thin flux tubes Convective instability of thin flux tubes

May 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979soph...62...15s&link_type=abstract

Solar Physics, vol. 62, May 1979, p. 15-22.

Physics

116

Convective Flow, Magnetic Flux, Magnetohydrodynamic Stability, Solar Magnetic Field, Surface Stability, Approximation, Buoyancy, Gas Pressure, Linear Equations, Solar Physics, Thermodynamic Equilibrium

Scientific paper

The convective instability of a thin vertical flux tube is examined. The thin-tube approximation of the MHD equations is used, and a linear stability analysis is performed. The value of the critical magnetic-field strength at the solar surface, which distinguishes between stability and instability, is found to be 1350 G if beta is approximately constant over the depth range in which the force driving the instability acts (i.e., the first few hundred kilometers below the surface). Since the strength of the small-scale magnetic field in active regions is generally observed to be around 1000 G, it is concluded that the flux tubes that constitute this field are hydrodynamically stable. The fate of an unstable flux tube is briefly considered.

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