Physics
Scientific paper
Oct 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978soph...59..249w&link_type=abstract
Solar Physics, vol. 59, Oct. 1978, p. 249-274. Research supported by the University of St. Andrews.
Physics
73
Convection, Magnetic Flux, Magnetohydrodynamic Stability, Solar Atmosphere, Solar Magnetic Field, Astronomical Models, Flow Stability, Photosphere, Temperature Profiles
Scientific paper
The nature of convective instability in a slender magnetic flux tube is considered, and a sufficient condition for stability is derived for the case of an arbitrary temperature profile in the external medium. The approach permits the existence of a temperature difference between the interior and exterior of the tube. The distribution of stable and unstable eigenvalues for a linear temperature profile is examined in detail. The model suggests that intense flux tubes are convectively stable if sufficiently shallow (depth 1000-2000 km or less). Downdrafts observed inside intense flux tubes might be a transient phenomenon in which the field inside the tube is further intensified until hydrostatic equilibrium occurs. It is concluded that convective instability in a flux tube is a possible means of achieving kilogauss field strengths.
Roberts Barney B.
Webb Richard A.
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