Convective instability in a solar flux tube. I - Nonlinear calculations for an adiabatic inviscid fluid

Details Convective instability in a solar flux tube. I - Nonlinear calculations for an adiabatic inviscid fluid Convective instability in a solar flux tube. I - Nonlinear calculations for an adiabatic inviscid fluid

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...285..851s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 285, Oct. 15, 1984, p. 851-857.

Astronomy and Astrophysics

Astrophysics

42

Convective Heat Transfer, Magnetohydrodynamic Stability, Solar Flux, Solar Magnetic Field, Inviscid Flow, Oscillating Flow, Perturbation Theory, Photosphere, Sunspots

Scientific paper

The temporal evolution of a slender flux tube extending vertically in the convection zone of the sun is modeled by numerical solution of the MHD equations. Initial states in hydrostatic equilibrium and for which beta (the ratio of the thermal to magnetic pressure at the initial epoch) is constant with depth are considered. The time-dependent response of these states to a velocity perturbation is examined. When the perturbation is a downflow, convective collapse of the flux tube occurs when beta is approximately equal to or larger than 2. The numerical solutions are followed for long enough times for the instability to be quenched. An important finding to emerge is that the final state is not a steady one, but rather a stationary oscillating one. The surface magnetic field in the final state has an average value of about 1400 G, with an oscillating amplitude of about 200 G. There is an oscillating flow with an amplitude of about 600 m/s with an average value that is approximately zero. The observational implications of these results are discussed.

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