Abstract
The rotation of the solar corona has been studied using recurrence properties of the green coronal line (5303 Å) for the interval 1947–1970. Short-lived coronal activity is found to show the same differential rotation as short-lived photospheric magnetic field features. Long-lived recurrences show rigid rotation in the latitude interval ±57°.5. It is proposed that at least part of the variability of rotational properties of the solar atmosphere may be understood as a consequence of coexistence of differential and rigid solar rotation.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Howard, R. and Harvey, J.: 1970, Solar Phys. 12, 23.
Newton, H. W. and Nunn, M. L.: 1951, Monthly Notices Roy. Astron. Soc. 111, 413.
Svalgaard, L.: 1972, J. Geophys. Res. 77, 4027.
Wilcox, J. M. and Howard, R.: 1968, Phys. Rev. Letters 20, 1252.
Wilcox, J. M. and Howard, R.: 1970, Solar Phys. 13, 251.
Wilcox, J. M. and Svalgaard, L.: 1974, to be published in Solar Physics.
Wilcox, J. M. and Tannenbaum, A. S.: 1971, Space Sci. Lab. Rep., Ser. 12, 45, University of California, Berkeley.
Wilcox, J. M., Schatten, K. H., and Tannenbaum, A. S.: 1970, Solar Phys. 14, 255.
Author information
Authors and Affiliations
Additional information
On leave from Torino University, Italy, as an ESRO-NASA Fellow.
Rights and permissions
About this article
Cite this article
Antonucci, E., Svalgaard, L. Rigid and differential rotation of the solar corona. Sol Phys 34, 3–10 (1974). https://doi.org/10.1007/BF00149592
Received:
Revised:
Issue Date:
DOI: https://doi.org/10.1007/BF00149592