The nonlinear evolution of a convective instability in a solar magnetic flux tube

Details The nonlinear evolution of a convective instability in a solar magnetic flux tube The nonlinear evolution of a convective instability in a solar magnetic flux tube

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasj...45..811t&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan, vol. 45, no. 6, p. 811-817

Astronomy and Astrophysics

Astronomy

6

Magnetic Flux, Magnetohydrodynamics, Solar Magnetic Field, Flux Density, Stability

Scientific paper

One-dimensional magnetohydrodynamic (MHD) numerical simulations were performed to study the nonlinear evolution of a convective instability within a vertical magnetic flux tube embedded in a layer extending from the solar photosphere to the convection zone. The thin flux tube approximation and adiabatic energy equation were assumed; the effect of ionization was included. We investigated how the results depend on the boundary condition (open or closed) at the lower boundary. The results are: (1) When the closed boundary condition is adopted at the lower boundary, a nonlinear oscillation is excited. The oscillation period increases with the depth of the lower boundary. (2) When an open boundary condition is assumed at the lower boundary, there is no nonlinear oscillation, and a new dynamic equilibrium is achieved, characterized by an intense (1kG) magnetic flux tube. We show that the nonlinear oscillation in case (1), which was reported previously (Hasan 1984), results from the reflection of a slow-mode MHD wave at the closed lower boundary. Since there is no closed boundary in an actual flux tube, our results imply that an intense flux tube may be created without generating nonlinear oscillations.

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