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The Toroidal Magnetic Field inside the Sun

Published online by Cambridge University Press:  12 April 2016

V.N. Krivodubskij ,
A.E. Dudorov ,
A.A. Ruzmaikin  and
T.V. Ruzmaikina
V.N. Krivodubskij
Affiliation:
Kiev University Astronomical Observatory, Kiev, 252053, U.S.S.R.
A.E. Dudorov
Affiliation:
Moscow UniversityAstronomy Department, Moscow, 117899, U.S.S.R.
A.A. Ruzmaikin
Affiliation:
IZMIRAN, Troitsk, Moscow region, 142092, U.S.S.R.
T.V. Ruzmaikina
Affiliation:
Institute of Physics of Earth, Moscow, 123810, U.S.S.R.

Extract

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Analysis of the fine structure of the solar oscillations has enabled us to determine the internal rotation of the Sun and to estimate the magnitude of the large-scale magnetic field inside the Sun. According to the data of Duvall et al. (1984), the core of the Sun rotates about twice as fast as the solar surface. Recently Dziembowski et al. (1989) have showed that there is a sharp radial gradient in the Sun’s rotation at the base of the convection zone, near the boundary with the radiative interior. It seems to us that the sharp radial gradients of the angular velocity near the core of the Sun and at the base of the convection zone, acting on the relict poloidal magnetic field Br, must excite an intense toroidal field Bф, that can compensate for the loss of the magnetic field due to magnetic buoyancy.

Type
Part III Solar magnetism and large-scale flows
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 187 - 189
Copyright
Copyright © Springer-Verlag 1991

References

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