𝔖 Bobbio Scriptorium
✦   LIBER   ✦

The solar photospheric abundance of iron

✍ Scribed by E. Biémont; N. Grevesse

Publisher
Springer
Year
1975
Tongue
English
Weight
467 KB
Volume
45
Category
Article
ISSN
0038-0938

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✦ Synopsis

A new value of the solar photospheric abundance of iron, independent of line-shape parameters, is derived. Our analysis is based on a study of 40 weak infrared lines (0.85<2<2.5/-0 for which theoretical oscillator strengths (calculated with configuration interactions taken into account) have recently been computed by Kurucz (1974). The abundance obtained, A Fe = 7.57:k0.11 (in the usual scale where logNr~ = 12.00) is in agreement with the 'high' solar values recently reported in the literature and with the meteoritic abundance.

📜 SIMILAR VOLUMES

Computation of oscillator strengths by a
Computation of oscillator strengths by a semiempirical method for some elements of the iron group and their solar photospheric abundance
✍ E. Biémont 📂 Article 📅 1974 🏛 Springer 🌐 English ⚖ 184 KB

Absolute oscillator strengths are computed by the STF method for selected lines of Scl.The lifetimes deduced from these values are in satisfactory agreement with recent beam-foil measurements. From a study of 10 selected lines, a new value of the solar photospheric abundance is derived (logNsc = 3.0

Computation of oscillator strengths by a
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✍ E. Biémont 📂 Article 📅 1974 🏛 Springer 🌐 English ⚖ 793 KB

Oscillator strengths are calculated for 259 lines of Ti I by taking configuration interaction into account in a somewhat simplified treatment. Radial integrals are obtained by an adaptation of the scaled Thomas-Fermi method. The great majority of selected lines originate from slightly perturbed term

Computation of oscillator strengths by a
Computation of oscillator strengths by a semi-empirical method for some elements of the iron-group and their solar photospheric abundance
✍ E. Biémont 📂 Article 📅 1978 🏛 Springer 🌐 English ⚖ 416 KB

Oscillator strengths calculated by the STF method for selected transitions of V I and Co I have permitted to deduce, from an LTE study of weak lines, photospheric abundances in agreement with those obtained from carbonaceous chondrites. A summary of results is also presented for all the iron-group e