Advertisement

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

  • J. O. Stenflo
Conference paper
Part of the International Astronomical Union book series (IAUS, volume 138)

Abstract

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 phaae velocity also represents the plasma velocity.

Keywords

Magnetic Flux Solar Cycle Rotation Rate Rotation Period Convection Zone 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. 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
  2. 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.ADSCrossRefGoogle Scholar
  3. 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.ADSCrossRefGoogle Scholar
  4. LaBonte, B.J. and Howard, R. (1982) ‘Torsional waves on the sun and the activity cycle’, Solar Phys. 75, 161–178.ADSCrossRefGoogle Scholar
  5. Martin, S.F. (1989) ‘Evolution of small-scale magnetic fields’, in these proceedings.Google Scholar
  6. Rüdiger, G. and Tuominen, I. (1989) ‘Generators of solar differential rotation and implications of lielioseismology’, in these proceedings.Google Scholar
  7. Schüssler, M. (1987) ‘Magnetic fields and the rotation of the solar convection zone’, in B.R. Durney and S. Sofia (eds.), The Internal Solar Angular Velocity, Astrophys. Space Sci. Library 137, 303–320.ADSGoogle Scholar
  8. 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.ADSCrossRefGoogle Scholar
  9. Snodgrass, H.B. (1983) ‘Magnetic rotation of the solar photosphere’, Astrophys. J. 270, 288–299.ADSCrossRefGoogle Scholar
  10. Spiegel, E.A. and Weiss, N.O. (1980) ‘Magnetic activity and variations in solar luminosity’, Nature 287, 616–617.ADSCrossRefGoogle Scholar
  11. Stenflo, J.O. (1988) ‘Global wave patterns in the Sun’s magnetic field’, Astrophys. Space Sci. 144, 321–336.ADSGoogle Scholar
  12. Stenflo, J.O. (1989) ‘Differential rotation of the Sun’s magnetic field pattern’, Astron. Astrophys. 210, 403–409.ADSGoogle Scholar
  13. Van Tend, W. and Zwaan, C. (1976) ‘On differences in differential rotation’, in V. Bumba and J. Kleczek (eds.), Basic Mechanisms of Solar Activity, IAU Symp. 71, 45–46.ADSGoogle Scholar

Copyright information

© International Astronomical Union 1990

Authors and Affiliations

  • J. O. Stenflo
    • 1
  1. 1.Institute of AstronomyZürichSwitzerland

Personalised recommendations