Abstract
Recent developments in solar dynamo and other theories of magnetic fields and convection are discussed and extended. A basic requirement of these theories, that surplus fields are eliminated by turbulent or eddy diffusion, is shown to be invalid. A second basic requirement, that strong surface fields are created by granule or supergranule motions, is shown to be improbable. Parker's new ‘thin-filament’ dynamo, based on the Petschek mechanism, is shown to provide the alternative possibilities: either the magnetic fields halt all convection or a steady state is reached in which the fields are a tangle of long, thin filaments. From the above and other considerations it is concluded that the dynamo and related diffuse-field theories are unacceptable, that solar magnetic fields are not dominated by convection, and that all the fields emerge as strong, concentrated fields (flux ropes) which were wound and twisted from a permanent, primordial field. The discussion may, incidentally, provide the physical elements of a deductive theory of hydromagnetic convection.
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References
Beckers, J. M. and Schröter, E. H.: 1968,Solar Phys. 4, 142.
Clark, A. and Johnson, A. C.: 1967,Solar Phys. 2, 433.
Dunn, R. B. and Zirker, J. B.: 1973,Solar Phys. 33, 281.
Elsasser, W.: 1956,Rev. Mod. Phys. 28, 135.
Elste, G.: 1973,Trans. IAU 15A, 130.
Frazier, E. N. and Stenflo, J. O.: 1972,Solar Phys. 27, 330.
Gubbins, D.: 1974,Rev. Geophys. Space Phys. 12, 137.
Harvey, J. W. and Hall, D.: 1974,Bull. Am. Astron. Soc. 6, 81.
Leighton, R. B.: 1964,Astrophys. J. 140, 1547.
Leighton, R. B.: 1969,Astrophys. J. 156, 1.
Livingston, W. C. and Harvey, J.: 1975, A.A.S. Solar Physics Division Meeting, Boulder, Colorado.
Mehltretter, J. P.: 1974,Solar Phys. 38, 43.
Meyer, F., Schmidt, H. U., Weiss, N. O., and Wilson, P. R.: 1974,Monthly Notices Roy. Astron Soc. 169, 35.
Moss, D. L.: 1970,Monthly Notices Roy. Astron. Soc. 148, 173.
Nakagawa, Y. and Priest, E. R.: 1973,Astrophys. J. 179, 949.
Osterbrock, D. E.: 1961,Astrophys. J. 134, 347.
Parker, E. N.: 1963,Astrophys. J. 138, 552.
Parker, E. N.: 1970,Ann. Rev. Astron. Astrophys. 8, 1.
Parker, E. N.: 1971,Astrophys. J. 162, 665;163, 279.
Parker, E. N.: 1973a,Astrophys. Space Sci. 22, 279.
Parker, E. N.: 1973b,Astrophys. J. 180, 247.
Parker, E. N.: 1973c,Astrophys. J. 186, 643, and 665.
Piddington, J. H.: 1971,Proc. Astron. Soc. Australia 2, 7.
Piddington, J. H.: 1972,Solar Phys. 22, 3.
Piddington, J. H.: 1973,Astrophys. Space Sci. 24, 259.
Piddington, J. H.: 1974, in R. G. Athay (ed.), ‘Chromospheric Fine Structure’,IAU Symp. 56, 269.
Piddington, J. H.: 1975a,Astrophys. Space Sci. 34, 347.
Piddington, J. H.: 1975b,Astrophys. Space Sci., in press.
Ponomarenko, Yu. B.: 1972,Astron. Zh. 49, 148, and 568;Astron. J. 16, 116 and 460.
Rädler, K.H.: 1968,Z. Naturforsch. 23a,1851.
Sheeley, N. R.: 1967,Solar Phys. 1, 171.
Simon, G. W. and Leighton, R. B.: 1964,Astrophys. J. 140, 1120.
Simon, G. W. and Weiss, N. O.: 1968,Z. Astrophys. 69, 435.
Stenflo, J. O.: 1973,Solar Phys. 32, 41.
Stix, M.: 1974,Astron. Astrophys. 37, 121.
Vainshtein, S. I. and Zel'dovich, Ya. B.: 1972,Usp. Fiz. Nauk 106, 431;Soviet Fiz. Usp. 15, 159.
Vrabec, D.: 1971, in R. Howard (ed.), ‘Solar Magnetic Fields’,IAU Symp. 43, 329.
Weiss, N. O.: 1966,Proc. Royal Soc. London. A293, 310.
Weiss, N. O.: 1971, in R. Howard (ed.), ‘Solar Magnetic Fields’,IAU Symp 43, 757.
Wilson, P. R.: 1972,Solar Phys. 22, 434;27, 363.
Yeh, T. and Axford, W. I.: 1970,J. Plasma Phys. 4, 207.
Yeh, T. and Dryer, M.: 1973,Astrophys. J. 182, 301.
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Piddington, J.H. Solar magnetic fields and convection. Astrophys Space Sci 38, 157–166 (1975). https://doi.org/10.1007/BF00646104
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DOI: https://doi.org/10.1007/BF00646104