Computer Science
Scientific paper
Nov 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984esasp.220...81m&link_type=abstract
In ESA The Hydromagnetics of the Sun p 81-84 (SEE N85-25091 14-92)
Computer Science
Convection, Magnetic Flux, Solar Activity Effects, Solar Cycles, Solar Magnetic Field, Atmospheric Stratification, Solar Atmosphere, Stellar Cores, Stellar Models
Scientific paper
The nonlinear development of the kink instability of a magnetic flux tube initially lying in mechanical equilibrium in the deep convection zone is presented. The unstable evolution is started by a small-amplitude sinusoidal perturbation of the shape of the flux tube in a vertical plane. As a result of the development of the instability, the lower part of the flux tube enters the radiative core and remains there confined within a fraction of the uppermost pressure scale-height of this region. The rising part of the flux tube crosses the convection zone in a dynamic time-scale of several weeks to a few months, and reaches the photosphere. A numerical code which calculates the dynamic evolution of a thin magnetic flux tube in the convection zone was developed. The code is lagrangian and allows for the compressibility of matter in the flux tube; for convection zone stratification the Spruit (1977) model is used.
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