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High dispersion spectroscopy of quiescent prominences

✍ Scribed by Lawrence W. Ramsey


Publisher
Springer
Year
1977
Tongue
English
Weight
609 KB
Volume
51
Category
Article
ISSN
0038-0938

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πŸ“œ SIMILAR VOLUMES


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✍ S. B. Pikel'ner πŸ“‚ Article πŸ“… 1971 πŸ› Springer 🌐 English βš– 370 KB

For stable equilibrium, prominences must be supported with magnetic lines of force leaning

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Quiescent prominences occur as long-lasting cool sheets of matter in the surrounding hot corona at the base of coronal streamers. Seen on the disk they appear as dark filaments dividing regions of opposite magnetic polarity. In this paper a theoretical model is presented, which describes the genera

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We present 2-D numerical models of quiescent solar prominences with normal magnetic polarity. These models represent an extension to the classical Kippenhahn-Schltiter model in that the prominence is treated as having finite width and height and the external coronal field is matched smoothly to the

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We present a simple magnetostatic theory of the thin vertical filaments that make up the quiescent prominence plasma as revealed by fine spatial resolution Ha photographs. A class of exact equilibrium solutions is obtained describing a horizontal row of long vertical filaments whose weights are supp

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A quiescent prominence has been observed with the MSDP spectrograph at the Pic du Midi Observatory. He profiles are obtained simultaneously in a 2D field, allowing a statistical analysis. The standard deviations of Doppler shifts and line widths are investigated as functions of the line intensity. T