𝔖 Bobbio Scriptorium
✦   LIBER   ✦

On the interpretation of the π-component splitting in sunspot spectra

✍ Scribed by V. N. Obridko; L. B. Demkina

Publisher
Springer
Year
1972
Tongue
English
Weight
294 KB
Volume
24
Category
Article
ISSN
0038-0938

No coin nor oath required. For personal study only.

✦ Synopsis

It is shown that in order to explain the observed splitting of the n-component in the sunspot umbra spectrum by the hypothesis of the coexistence in sunspots of weak-and strong-field regions with opposite polarities, one has to admit the additional assumption that in the weak-field regions the Doppler halfwidth (A~.D) and the ratio between line opacity and continuum opacity 0/0) are both less than those in the strong-field regions.

📜 SIMILAR VOLUMES

The Anomalous Splitting of the π-compone
The Anomalous Splitting of the π-component of a ZEEMAN Triplet in Sunspot Umbrae and Suggestions for its Interpretation
✍ H. KÜNZEL; J. Staude 📂 Article 📅 1975 🏛 John Wiley and Sons 🌐 English ⚖ 545 KB

## Abstract ZEEMAN‐Spektrogramme von 1200 Sonnenflecken aus dem Maximumjahr 1957 wurden ausgewertet, um die anomale Aufspaltung der π‐Komponente (d. h. deren relative Verschiebung in den Spektren __I__ + __V__ und __I__ ‐ __V__) der Linie Fe I 6302.5 Å in Umbren zu untersuchen. In Umbren mit magnet

On the interpretation of some peculiarit
On the interpretation of some peculiarities observed in zeeman-split line contours in sunspots
✍ Jürgen Staude 📂 Article 📅 1973 🏛 Springer 🌐 English ⚖ 256 KB

Strong line wings and the V-reversal in umbral countours of Fe~ 6302.5/~ and similar lines have been explained earlier by inhomogeneous magnetic models. It is shown that both effects may also be explained assuming a homogeneous magnetic field and homogeneous umbral model atmospheres. A discussion o

The possible presence of C2lines in suns
The possible presence of C2lines in sunspot spectra
✍ D. L. Lambert; E. A. Mallia 📂 Article 📅 1973 🏛 Springer 🌐 English ⚖ 216 KB

Indirect evidence against the presence of C2 lines in umbral spectra is discussed. The dominant role of CO in the molecular equilibrium of C at umbral temperatures ensures that CN, CH and Cz lines are formed in the same atmospheric regions. Observations of CN and CH umbral lines are in good accord w