𝔖 Bobbio Scriptorium
✦   LIBER   ✦

The Chromosphere Line λ 6676.9

✍ Scribed by YOUNG, C. A.

Book ID
109420901
Publisher
Nature Publishing Group
Year
1891
Tongue
English
Weight
133 KB
Volume
45
Category
Article
ISSN
0028-0836

No coin nor oath required. For personal study only.

📜 SIMILAR VOLUMES

Chromospheric oscillations observed in t
Chromospheric oscillations observed in the line Ciiλ1336 with OSO-8
✍ Eric G. Chipman 📂 Article 📅 1977 🏛 Springer 🌐 English ⚖ 473 KB

Satellite observations of velocity and intensity oscillations were made of the upper chromospheric line C tt A 1336. The dominant period of oscillation is 300 s, with little evidence of the power peak in the range 150-200 s which has been observed in other chromospheric lines. Peak-to-peak amplitude

λ 4097.3 Niiiemission in the chromospher
λ 4097.3 Niiiemission in the chromospheric spectrum?
✍ D. L. Lambert 📂 Article 📅 1971 🏛 Springer 🌐 English ⚖ 187 KB

The recent tentative identification of a chromospheric emission line at 2| : 4097.342/~ with the Nm transition 3s "2S1/., --3p ~P~ is discussed. It is shown that the observed intensity is inconsistent with the observed flux in the XUV resonance lines and considerably greater than the predicted inten

Line intensities in the photosphere-chro
Line intensities in the photosphere-chromosphere transition region
✍ E. L. Dessel 📂 Article 📅 1974 🏛 Springer 🌐 English ⚖ 806 KB

We analyse Fe i lines observed during the 1961 eclipse at Bra6, Yugoslavia (see paper II: van Dessel et aL, 1973), using a computer program for the calculation of theoretical line intensities, which was described in Paper I (van Dessel, 1970). A few minor modifications to the physical input are disc

Line intensities in the photosphere-chro
Line intensities in the photosphere-chromosphere transition region
✍ E. L. Dessel 📂 Article 📅 1975 🏛 Springer 🌐 English ⚖ 639 KB

Eclipse observations of total line intensities (Cr ~: two groups of lines; Ti II, Fe II and Cr iI: two lines each) are interpreted in terms of departures from LTE. The same method as described in Paper III is used. The HSRA model is used to compute the LTE populations. A distribution of NLTE-coeffi