Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasj...47..331t&link_type=abstract
PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 47, no. 3, p. 331-336
Astronomy and Astrophysics
Astronomy
5
Magnetic Flux, Magnetohydrodynamics, Photosphere, Solar Atmosphere, Solar Convection (Astronomy), Solar Magnetic Field, Stability, Algorithms, Computerized Simulation, Plasma Oscillations, Radiative Heat Transfer
Scientific paper
One-dimensional magnetohydrodynamic (MHD) numerical simulations were performed in order to investigate the convective stability of an intense photospheric flux tube, adopting the thin flux-tube approximation. The radiative heat exchange between the flux tube and its surroundings was also taken into account using Newton's law of cooling. To study the stability, we examined the temporal evolution of a small perturbation (downflow) added to an initial atmosphere. When a closed-boundary condition is adopted at the lower boundary, the perturbation evolves into a longitudinal overstable oscillation. However, an open (flow-through) condition at the lower boundary should be more suitable for representing the actual solar conditions, because a closed condition excludes the leakage of perturbations, through the boundary. We thus repeated the simulation while adopting an open condition for the lower boundary. As a result, it was shown that the perturbation does not evolve into an overstable oscillation, but, rather, leaks out completely through the lower boundary. Our results imply that the actual photospheric flux tubes are in a convectively stable state, consistent with the recent observational results.
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