Abstract
A continuous relationship is proposed between the basic elements of the dark fine structure of the quiet and active chromosphere. A progression from chromospheric bushes to fibrils, then to chromospheric threads and active region filaments, and finally to diffuse quiescent filaments, is described. It is shown that the horizontal component of the field on opposite sides of an active region quiescent filament can be in the same direction and closely parallel to the filament axis. Consequently, it is unnecessary to postulate twisted or otherwise complex field configurations to reconcile the support mechanism of filaments with the observed motion along their axis.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Bruzek, A.: 1969, Solar Phys. 8, 129.
Howard, R. and Harvey, J. W.: 1964, Astrophys. J. 139, 1328.
Kiepenheuer, K. O.: 1967, in Solar Physics (ed. by Xanthakis), Interscience.
Rust, D. M.: 1967, Astrophys. J. 150, 313.
Smith, S. F.: 1968, in K. O. Kiepenheuer (ed.) ‘Structure and Development of Solar Active Regions’, IAU Symp. 35, 267.
Weart, S. R.: 1970, Astrophys. J., 162, 987.
Zirin, H.: 1970, Sky Telesc. 39, 215.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Foukal, P. Morphological relationships in the chromospheric Hα fine structure. Sol Phys 19, 59–71 (1971). https://doi.org/10.1007/BF00148824
Received:
Revised:
Issue Date:
DOI: https://doi.org/10.1007/BF00148824