We have measured the longitudinal component, Bll, of the magnetic field in quiescent prominences and obtained a relationship between BII and 0, where 0 is the angle between the long axis of the prominence and the north-s0uth direction on the sun. From this relationship we deduce a distribution funct
Remarks on the magnetic support of quiescent prominences
β Scribed by U. Anzer; E. Priest
- Publisher
- Springer
- Year
- 1985
- Tongue
- English
- Weight
- 301 KB
- Volume
- 95
- Category
- Article
- ISSN
- 0038-0938
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β¦ Synopsis
The development of magnetic field structures which can lead to prominence configurations of the Kuperus-Raadu type is discussed. Starting from streamer type configurations and preserving the total current in the system we find that simple two-dimensional static configurations lead to prominences which in general lie systematically much lower than the heights found from observations. We therefore conclude that either more complex field configurations are needed to explain the recent observations by Leroy et aL (1983) or the initial configurations must be very special.
π SIMILAR VOLUMES
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
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