Abstract
Although magnetic convection in all probability does operate inside the Sun, the energy flux which it can carry is 5–6 orders of magnitude smaller than the total solar flux. Thus the effects of magnetic convection on the internal temperature structure of the Sun are probably small.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Davis, R.: 1972, Bull. Am. Phys. Soc. 17, 527.
Gurm, H. S. and Wentzel, D. G.: 1967, Astrophys. J. 149, 139.
Iben, I.: 1967, Ann. Rev. Astron. Astrophys. 5, 586.
Mullan, D. J.: 1973, Astrophys. J. 186, 1059.
Parker, E. N.: 1974, ‘The Instability of Strong Magnetic Fields in Stellar Interiors’, preprint.
Schatten, K. H.: 1973, Solar Phys. 33, 305.
Schwarzschild, M.: 1958, Structure and Evolution of the Stars, Princeton Univ. Press, pp. 51, 359.
Sturrock, P. A. and Gilvarry, J. J.: 1967, Nature 216, 1280.
Ulrich, R. K.: 1974, Astrophys. J. 188, 369.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Mullan, D.J. Is magnetic convection important in the Sun?. Sol Phys 38, 9–13 (1974). https://doi.org/10.1007/BF00161819
Received:
Revised:
Issue Date:
DOI: https://doi.org/10.1007/BF00161819