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Large-Scale Internal Magnetic Field of the Sun

Published online by Cambridge University Press:  08 February 2017

A.E. Dudorov ,
V.N. Krivodubskij ,
A.A. Ruzmaikin  and
T.V. Ruzmaikina
A.E. Dudorov
Affiliation:
1Astronomy Department of Moscow State University 117899, Moscow, USSR
V.N. Krivodubskij
Affiliation:
2Kiev Shevchenko University Astronomical Observatory 252053, Kiev, USSR
A.A. Ruzmaikin
Affiliation:
3IZMIRAN, 142092, Troitsk, Moscow region, USSR
T.V. Ruzmaikina
Affiliation:
4Institute of Physics of Earth, 123810, Moscow, USSR

Abstract

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The behaviour of the magnetic field during the formation and evolution of the Sun is investigated. It is shown that an internal poloidal magnetic field of the order of 104 − 105 G near the core of the Sun may be compatible with differential rotation and with torsional waves, travelling along the magnetic field lines (Dudorov et al., 1989).

Type
VI. Generation of Solar Magnetic Fields
Information
Symposium - International Astronomical Union , Volume 138: Solar Photosphere: Structure, Convection and Magnetic Fields , 1990 , pp. 391 - 394
Copyright
Copyright © Kluwer 1990 

References

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