The Dynamical Oscillation and Propulsion of Magnetic Fields in the Convective Zone of a Star. III. Accumulation of Heat and the Onset of the Reyleigh-Taylor Instability

Details The Dynamical Oscillation and Propulsion of Magnetic Fields in the Convective Zone of a Star. III. Accumulation of Heat and the Onset of the Reyleigh-Taylor Instability The Dynamical Oscillation and Propulsion of Magnetic Fields in the Convective Zone of a Star. III. Accumulation of Heat and the Onset of the Reyleigh-Taylor Instability

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...321.1009p&link_type=abstract

Astrophysical Journal v.321, p.1009

Astronomy and Astrophysics

Astronomy

14

Instabilities, Stars: Interiors, Sun: Interior, Hydromagnetics

Scientific paper

This paper studies the time-dependent accumulation of heat beneath a thermal barrier simulating a broad band of intense azimuthal field in the lower convective zone of the Sun, or other star. The accumulating heat causes the gas density beneath the field to decline (Δρ/ρ = -ΔT/T) to the point that the gas is less dense than the gas within the magnetic field (where Δρ/ρ = -β2/8πp). The resulting Rayleigh-Taylor instability causes tongues of heated gas to penetrate upward through the field. We suggest that the tongues of hot gas take on the nature of thermal plumes, extending all the way to the surface, where they provide the emerging magnetic fields that give rise to the activity of the Sun. The whole process, beginning with the accumulation of heat, followed by the onset of the Rayleigh-Taylor instability, and the extension of tongues of hot gas into thermal plumes to the surface, is estimated to take a week or two, in agreement with the observed weekly emergence of thermal plumes and magnetic flux in activity complexes at the surface.

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