Hostname: page-component-77c89778f8-sh8wx Total loading time: 0 Render date: 2024-07-20T06:19:32.116Z Has data issue: false hasContentIssue false
  • English
  • Français

Filament Channels: Contrasting Their Structure in Hα and He I 1083 nm

Published online by Cambridge University Press:  12 April 2016

Karen L. Harvey  and
Victor Gaizauskas
Karen L. Harvey
Affiliation:
Solar Physics Research Corporation, 4720 Calle Desecada, Tucson, AZ 85718, U.S.A.
Victor Gaizauskas
Affiliation:
Herzberg Institute of Astrophysics, National Research Council, 100 Sussex Drive, Ottawa, CanadaK16OR6

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

From a direct comparison, we find that filament channels are more easily detected in He I λ1083 than in Hλ, particularly for polar crown filaments. He I 1083 nm filament channels appear to coincide with the outer boundaries of Yohkoh/SXT X-ray cavities.

Type
Birth and Death of Filaments
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 269 - 273
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Foukal, P. 1971, Solar Phys., 19, 59 CrossRefGoogle Scholar
Hudson, H.S., Acton, L.A. and Harvey, K.L. 1998, to be submittedGoogle Scholar
Martin, S.F., Bilimoria, R. and Tracadas, P.W. 1994, in Solar Surface Magnetism, (eds.) Rutten, R. J. and Schrijver, C. J., Kluwer Acad. Publ., Dordrecht, Holland, p. 303 CrossRefGoogle Scholar
Serio, S, Vaiana, G.S., Godoli, G., Motta, S., Pirronello, V. and Zappala, R.A. 1978, in Proceedings of the Open Meetings of the Working Groups on Physical Sciences, Tel Aviv, Israel, Oxford, Pergamon Press, p. 337 Google Scholar
Tandberg-Hanssen, E. 1974, Solar Prominences, D. Reidel Publishing Co., Dordrecht, Holland, p. 132 CrossRefGoogle Scholar