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
The formation of solar quiescent prominences by condensation
β Scribed by E. Hildner
- Publisher
- Springer
- Year
- 1974
- Tongue
- English
- Weight
- 760 KB
- Volume
- 35
- Category
- Article
- ISSN
- 0038-0938
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