Generation of Torsional Oscillations in the Sun

  • Y. V. Vandakurov
Conference paper
Part of the International Astronomical Union book series (IAUS, volume 138)

Abstract

The hypothesis is considered that the torsional wave observed on the Sun is an eigenmode oscillation excited in the presence of a weak poloidal magnetic field. We derive asymptotic linear equations for a perturbation with a large number of nodes along the radius, assuming the rotation to be slow and the characteristic perturbation period to be much longer than the rotational period. The results of a preliminary numerical study of the stability of the torsional mode indicate that the superadiabaticity of the solar convection may contribute to the excitation of this mode. In the present work the approximation of harmonic radial dependence of the perturbation has been used.

Keywords

Solar Phys Convection Zone Torsional Oscillation Torsional Mode Toroidal Magnetic Field 
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Copyright information

© International Astronomical Union 1990

Authors and Affiliations

  • Y. V. Vandakurov
    • 1
  1. 1.A.F. Ioffe Physical Technical InstituteAcademy of Sciences of the USSRLeningradUSSR

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