Abstract
Coronal holes are extensive regions of extremely low density in the solar corona within 60° of latitude from the equator. (They are not to be confused with the well-known coronal cavities which surround quiescent prominences beneath helmet streamers.) We have superposed maps of the calculated current-free (potential) coronal magnetic field with maps of the coronal electron density for the period of November 1966, and find that coronal holes are generally characterized by weak and diverging magnetic field lines. The chromosphere underlying the holes is extremely quiet, being free of weak plages and filaments. The existence of coronal holes clearly has important implications for the energy balance in the transition region and the solar wind.
Article PDF
Similar content being viewed by others
Avoid common mistakes on your manuscript.
References
Altschuler, M. D. and Newkirk, G.: 1969, Solar Phys. 9, 131.
Altschuler, M. D. and Perry, R. M.: 1972, Solar Phys. 23, 410.
Bohlin, J. D.: 1970, Solar Phys. 13, 153.
Hansen, R. T., Hansen, S. F., Garcia, C. J., and Trotter, D. E.: 1971, Solar Phys. 18, 271.
Kuperus, M.: 1965, Res. Astron. Obs. Utrecht 17 (1), 1.
Newkirk, G. and Altschuler, M. D.: 1970, Solar Phys. 13, 131.
Osterbrock, D. E.: 1961, Astrophys. J. 134, 347.
Pneuman, G. W.: 1968, Solar Phys. 3, 578.
Pneuman, G. W.: 1969, Solar Phys. 6, 255.
Withbroe, G. L.: 1972, Solar Phys., in press.
Withbroe, G. L., Dupree, A. K., Goldberg, L., Huber, M. C. E., Noyes, R. W., Parkinson, W. H., and Reeves, E. M.: 1972, Solar Phys. 21, 272.
Author information
Authors and Affiliations
Additional information
The National Center for Atmospheric Research is sponsored by the National Science Foundation.
Rights and permissions
About this article
Cite this article
Altschuler, M.D., Trotter, D.E. & Orrall, F.Q. Coronal holes. Sol Phys 26, 354–365 (1972). https://doi.org/10.1007/BF00165276
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF00165276