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Solar Physics

, Volume 22, Issue 1, pp 3–19 | Cite as

Solar dynamo theory and the models of Babcock and Leighton

  • J. H. Piddington
Article

Abstract

The dynamo theory of the solar cycle as developed by Parker and others, and the observational models of Babcock and Leighton have been examined, with the conclusion that the dynamo theory is not applicable to the Sun and that the models fail.

An essential part of the theory is an adequate effective diffusion coefficient. Fields are continuously sheared and amplified and, in this theory, these may not be allowed to accumulate; all subsurface fields of an old cycle must be eliminated. Ohmic diffusion is negligible and turbulent diffusion is invoked. However, this requires that all solar fields are tangled to a small scale, which is contrary to observation; for Hale's polarity laws are strictly observed, and large-scale surface features are common at the end of an 11-yr cycle in the same general area where new fields are appearing.

The erupted (sunspot) fields lie generally above the unerupted, toroidal fields so that, even if they are merged as required, the centroid of the new system would be above that of the old. The result is not a steady-state oscillator, as required, but the complete loss of the solar field.

It is concluded that for these and other reasons a shallow, reversing field is unacceptable, and that a deeply penetrating field is required. Reference is made to an alternative theory of the solar cycle based on a deep magnetic field.

Keywords

Solar Cycle Complete Loss Effective Diffusion Alternative Theory Turbulent Diffusion 
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.

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References

  1. Allen, C. W.: 1963, Astrophysical Quantities, 2nd ed., Univ. of London.Google Scholar
  2. Babcock, H. W.: 1961, Astrophys. J. 133, 572.Google Scholar
  3. Braginskii, S. I.: 1964, Soviet Phys. - JETP 20, 726 and 1462.Google Scholar
  4. Brunner, W.: 1930, Astron. Mitt. Zürich, No. 124, p. 67.Google Scholar
  5. Bumba, V. and Howard, R. F.: 1965, Astrophys. J. 141, 1492 and 1502.Google Scholar
  6. Bumba, V., Howard, R., Martres, M. J., and Soru-Iscovici, I.: 1968, in K. O. Kiepenheuer (ed.), ‘Structure and Development of Solar Active Regions’, IAU Symp. 35, 13.Google Scholar
  7. Cowling, T. G.: 1957, Magnetohydrodynamics, Interscience, New York.Google Scholar
  8. de Jager, C.: 1959, Handbuch der Physik 52, 80.Google Scholar
  9. Gilman, P. A.: 1969, Solar Phys. 8, 316.Google Scholar
  10. Hale, G. E. and Nicholson, S. B.: 1938, Carnegie Inst. Wash. Publ., No. 498.Google Scholar
  11. Haurwitz, M. W.: 1968, Astrophys. J. 151, 351.Google Scholar
  12. Howard, R.: 1965, in R. Lüst (ed), ‘Stellar and Solar Magnetic Fields’, IAU Symp. 22, 129.Google Scholar
  13. Kiepenheuer, K. O.: 1953, The Sun, (ed. by G. P. Kuiper), Univ. of Chicago Press.Google Scholar
  14. Kiepenheuer, K. O.: 1970, Trans. IAU 14A, 77.Google Scholar
  15. Kraichnan, R. H. and Nagarajan, S.: 1967, Phys. Fluids 10, 859.Google Scholar
  16. Leighton, R. B.: 1964, Astrophys. J. 140, 1547.Google Scholar
  17. Leighton, R. B.: 1969, Astrophys. J. 156, 1.Google Scholar
  18. Parker, E. N.: 1955, Astrophys. J. 121, 491.Google Scholar
  19. Parker, E. N.: 1970a, Ann. Rev. Astron. Astrophys. 8, 1.Google Scholar
  20. Parker, E. N.: 1970b, Astrophys. J. 162, 665.Google Scholar
  21. Parker, E. N.: 1971a, Astrophys. J. 163, 279.Google Scholar
  22. Parker, E. N.: 1971b, Astrophys. J. 164, 491.Google Scholar
  23. Piddington, J. H.: 1971, Proc. Astron. Soc. Australia 2, 7.Google Scholar
  24. Ribes, E. and Unno, W.: 1971, Proc. Astron. Soc. Australia, 2, 54.Google Scholar
  25. Richardson, R. S. and Schwarzschild, M.: 1953, Accademia Nazionale Lincei, Convegno 11, Rome 1952.Google Scholar
  26. Spitzer, L.: 1968, Diffuse Matter in Space, Wiley-Interscience, New York.Google Scholar
  27. Steenbeck, M. and Krause, F.: 1969, Astron. Nachr. 291, 49.Google Scholar
  28. Ward, F.: 1965, Astrophys. J. 141, 534.Google Scholar
  29. Williams, I. P. and Cremin, A. W.: 1968, Quart. J. Roy. Astron. Soc. 9, 40.Google Scholar

Copyright information

© D. Reidel Publishing Company 1972

Authors and Affiliations

  • J. H. Piddington
    • 1
  1. 1.CSIRO Division of PhysicsNational Standards LaboratorySydneyAustralia

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