Computer Science – Numerical Analysis
Scientific paper
Mar 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995soph..157...31p&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 157, no. 1-2, p. 31-44
Computer Science
Numerical Analysis
7
Polarity, Solar Magnetic Field, Solar Physics, Sun, Wave Excitation, Wave Generation, Cartesian Coordinates, Magnetohydrodynamics, Numerical Analysis, Shear Flow, Wave Propagation
Scientific paper
In this paper an excitation of waves is considered during the time interval in which the undisturbed magnetic field changes its direction. If this interval is taken to be 2 years, which is shorter than the 11-year cycle, then the undisturbed components of the magnetic field may be linearly dependent on time and independent of the coordinates. The excitation of waves is due to the undisturbed stationary V0 flow with div V0 = 0 and with (V0 rot0) = constant. We use the local Cartesian coordinate system, which is immovable towards the solar center, and consider the case when the toroidal component of the undisturbed magnetic field changes its sign simultaneously with one of the axial components. The third component does not change its direction. The efficiency of the enhancement of the magnetic field and velocity disturbances depends on the Alfven wave frequency, omegaA. When omegaA = 0, the component of the disturbed velocity, which is directed along the constant component of the undisturbed magnetic field, increases. In this case the shear waves excite the carrier (high) frequency (KV0), where K is the wave vector. Due to the shear instability the amplitude of the velocity increases during 1 year before the moment of reversal of the global magnetic field polarity (RGMFP) for an arbitrary latitude. It reaches a maximum at RGMFP and decreases in the next year. When omegaA greater than 0, then the amplitudes of the disturbed values reach maxima before the moment of RGMFP, and when omega0 less than 0, they reach maxima after it. We argue that the shear waves propagate from middle latitudes to the pole and equator. Using the results of the analytical solutions and leaning on the evidence of the observational data, we derive the result that the component of the undisturbed magnetic field, which is perpendicular to the solar surface, changes its sugn simultaneously with the toroidal component.
Pataraya Avtandil D.
Zaqarashvili Teimuraz V.
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