Convective instability in a solar flux tube. II - Nonlinear calculations with horizontal radiative heat transport and finite viscosity

Details Convective instability in a solar flux tube. II - Nonlinear calculations with horizontal radiative heat transport and finite viscosity Convective instability in a solar flux tube. II - Nonlinear calculations with horizontal radiative heat transport and finite viscosity

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...143...39h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 143, no. 1, Feb. 1985, p. 39-45.

Astronomy and Astrophysics

Astrophysics

66

Convective Flow, Magnetic Flux, Magnetohydrodynamic Stability, Radiative Heat Transfer, Solar Magnetic Field, Viscosity, Nonlinearity, Photosphere, Solar Oscillations, Thermodynamic Equilibrium

Scientific paper

Convective instability in a thin flux tube is examined in the presence of horizontal radiative heat transport and finite viscosity. The temporal behaviour of flux tubes initially in hydrostatic and thermal equilibrium is studied by solving the nonlinear time dependent equations for a thin flux tube. An important result of the investigation is the demonstration of overstable oscillations with periods typically about 1000s in intense flux tubes on the Sun. Overstability is a direct consequence of radiative exchange between the flux tube and the surrounding medium. Detailed calculations are presented for a broad range of parameters which characterize the strength of the magnetic field and the tube radius in the intial state. An initial stratification based on a model atmosphere is used. The results indicate that that overstable oscillations are produced as an end state of the convective instability. It is found that the surface magnetic field that results is in the observed kG range. Furthermore, there is also an oscillating flow (unidirectional at any given instant) with an amplitude between 1 and 2 km s-1, with an average value that is approximately zero. The observational implications of these results are discussed.

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