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The Sun's Rotation Rate as Inferred from Magnetic Field Data

Published online by Cambridge University Press:  08 February 2017

J.O. Stenflo
J.O. Stenflo*
Affiliation:
Institute of Astronomy ETH-Zentrum, CH-8092 Zürich Switzerland

Abstract

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The pattern of solar magnetic fields has been used as a tracer to determine how the sun's rotation rate varies with latitude and time. Two distinctly different rotation laws emerge from such an analysis, one agreeing with the surface Doppler rotation rate, the other corresponding to much more rigid rotation with a small polar spin-up. Detailed analysis shows that this second law cannot be explained in terms of flux redistribution on the solar surface, but that it represents the rotation properties of the sources of magnetic flux, which are likely to be located at the bottom of the convection zone.

The rotational phase velocity of the source pattern is found to be constant with time, which suggests that the depth at which the magnetic flux is stored and amplified inside the sun does not vary with the solar cycle, and that the phase velocity also represents the plasma velocity.

Type
V. Large-scale Structure and Dynamics
Information
Symposium - International Astronomical Union , Volume 138: Solar Photosphere: Structure, Convection and Magnetic Fields , 1990 , pp. 309 - 314
Copyright
Copyright © Kluwer 1990 

References

DeLuca, E.E. (1987) ‘Dynamo theory for the interface between the convection zone and the radiative interior of a star’, NCAR Cooperative Thesis No. 104, Boulder, Colorado.Google Scholar
Howard, R. and LaBonte, B. (1980) ‘The Sun is observed to be a torsional oscillator with a period of 11 years’, Astrophys. J. 239, L33–L36.Google Scholar
Howard, R., Adkins, J.M., Boyden, J.E., Cragg, T.A., Gregory, T.S., LaBonte, B.J., Padilla, S.P., and Webster, L. (1983) ‘Solar rotation results at Mount Wilson’, Solar Phys. 83, 321–338.CrossRefGoogle Scholar
LaBonte, B.J. and Howard, R. (1982) ‘Torsional waves on the sun and the activity cycle’, Solar Phys. 75, 161–178.CrossRefGoogle Scholar
Martin, S.F. (1989) ‘Evolution of small-scale magnetic fields’, in these proceedings.Google Scholar
Rüdiger, G. and Tuominen, I. (1989) ‘Generators of solar differential rotation and implications of helioseismology’, in these proceedings.CrossRefGoogle Scholar
Schüssler, M. (1987) ‘Magnetic fields and the rotation of the solar convection zone’, in Durney, B.R. and Sofia, S. (eds.), The Internal Solar Angular Velocity, Astrophys. Space Sci. Library 137, 303–320.CrossRefGoogle Scholar
Sheeley, N.R. Jr., Nash, A.G., and Wang, Y.-M. (1987) ‘The origin of rigidly rotating magnetic field patterns on the sun’, Astrophys. J. 319, 481–502.CrossRefGoogle Scholar
Snodgrass, H.B. (1983) ‘Magnetic rotation of the solar photosphere’, Astrophys. J. 270, 288–299.Google Scholar
Spiegel, E.A. and Weiss, N.O. (1980) ‘Magnetic activity and variations in solar luminosity’, Nature 287, 616–617.CrossRefGoogle Scholar
Stenflo, J.O. (1988) ‘Global wave patterns in the Sun's magnetic field’, Astrophys. Space Sci. 144, 321–336.Google Scholar
Stenflo, J.O. (1989) ‘Differential rotation of the Sun's magnetic field pattern’, Astron. Astrophys. 210, 403–409.Google Scholar
Van Tend, W. and Zwaan, C. (1976) ‘On differences in differential rotation’, in Bumba, V. and Kleczek, J. (eds.), Basic Mechanisms of Solar Activity, IAU Symp. 71, 45–46.Google Scholar