The formation of the solar Call K-line core is studied under the assumption of a two component chromosphere for many atmosphere models, which are tested by comparing observed and calculated average intensity profiles at several places on the solar disk. Non-LTE-line profile calculations are made usi
The formation of the CaiiK line in a spinning spicule
โ Scribed by Lorne W. Avery
- Publisher
- Springer
- Year
- 1970
- Tongue
- English
- Weight
- 851 KB
- Volume
- 13
- Category
- Article
- ISSN
- 0038-0938
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โฆ Synopsis
The emission of the CaII K line from a spinning cylindrical spicule model is considered. In order to reproduce the observed spicule K line profiles, the model must have both radial and axial gradients in Ne and Te. The rotating spicule model is optically thin at all heights and is hotter and more dense than a stationary model computed in a previous paper. It is proposed that the so-called Type I and Type II spicules may be structurally the same features, with different rotational velocities.
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