To calculate the Balmer, Paschen, and Brackett line intensities, we solved the statistical equilibrium equations for a twenty level plus continuum atom of hydrogen. From the temperature, ionization, and the first three level populations of the prominence models deduced in a previous work we have ca
On the Balmer: Paschen ratio in prominences
โ Scribed by Jay M. Pasachoff; Eric J. Pilger; Stephen R. Platt
- Publisher
- Springer
- Year
- 1983
- Tongue
- English
- Weight
- 169 KB
- Volume
- 89
- Category
- Article
- ISSN
- 0038-0938
No coin nor oath required. For personal study only.
๐ SIMILAR VOLUMES
We present measurements of the middle Balmer decrement (n = 10-22) in a number of quiescent prominences. The average decrement continues smoothly the trend of the decrement determined in our previous work on the earlier Balmer lines. The range of Tex is found to be 3450-11 000 K, consistent with the
Spectroscopic observations of the Nal D emission lines of prominences were made with the Domeless Solar Telescope in Hida Observatory. When active prominences are bright in the D 2 emission line, the intensity ratio of D~ to D 2 is found to deviate significantly from the theoretical ratio of the opt