THE ABUNDANCES OF THE ELEMENTS IN THE SOLAR ATMOSPHERE

Journal Article · Tue Nov 01 04:00:00 UTC 1960 · Astrophysical Journal (U.S.)

DOI:https://doi.org/10.1086/190053· OSTI ID:4057149

Goldberg, L; Muller, E A; Aller, L H

The method of weighing functions was utilized to derive the abundances of forty-two elements from faint and medium-strong lines is the solar spectrum. The model atmosphere adopted was that of Aller and Pierce as extended by Elste to both higher and deeper layers. The chief sources of equivalent widths were the measurements by Allen and by the Utrecht astronomers, but a substantial number of new measurements were included from McMathHulbert Observatory data. The f-values were taken from many different sources, but, whenever possible, experimental measurememts were employed. When laboratory data were not available, they were replaced by theoretical values based on the assumption of LS coupllng and making; use of the f-sum rule or of the Bates and Damgaard tables for the absolute scale factor. A detailed description is given of the derivation of the abundance of each element, including the major sources of uncertainty, such as the errors in the measurement of weak lines throughout the spectrum and of all lines in the ultraviolet region, uncertainties in the solar model for ultraviolet lines, and tbe unreliable character of many of the f-values employed. (auth)

• Research Organization: Univ. of Michigan Observatory, Ann Arbor
• Sponsoring Organization: USDOE
• NSA Number: NSA-15-013559
• OSTI ID: 4057149
• Journal Information: Astrophysical Journal (U.S.), Journal Name: Astrophysical Journal (U.S.) Vol. Vol: 5: Suppl. Ser., No. 45; ISSN ASJOA
• Country of Publication: Country unknown/Code not available
• Language: English

Related Subjects

ASTROPHYSICS
ELEMENTS
ERRORS
LEVELS
MEASURED VALUES
MOMENTUM
PHYSICS
QUANTITY RATIO
QUANTUM MECHANICS
SPECTRA
SPECTROSCOPY
SPIN
SUN
ULTRAVIOLET RADIATION