Magnetohydrodynamic turbulence in the solar convective zone as a source of oscillations and sunspots formation

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Abstract

As was previously shown (Kleeorin et al. 1990; Kleeorin & Rogachevskii 1994a), small-scale magnetohydrodynamic (MHD) turbulence results in modification of the Ampere law, by significantly reducing the elasticity of the magnetic field lines. As a result, the 'effective' magnetic pressure is reduced and may even reverse its sign. We show here that this modification can be related to a variety of phenomena observed in the Sun and in particular the following four are investigated: the 11-year variations of the solar radius, the torsional oscillations and the meridional flows, the solar short time oscillations and the large-scale magnetic flux ropes formation in convective zones of the Sun (as well as in stars and spiral galaxies).

Original languageEnglish
Pages (from-to)293-309
Number of pages17
JournalAstronomy and Astrophysics
Volume307
Issue number1
StatePublished - 1 Mar 1996

Keywords

  • Instabilities
  • Magnetohydrodynamics (MHD)
  • Sun: oscillations
  • Sunspots
  • Turbulence

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