Edith A. Muller

The Abundances of the Elements in the Solar Atmosphere.

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)

The Vertical Distribution of Nitrous Oxide and Methane in the Earth’s Atmosphere*

The intensities of the atmospheric lines P25, P26, P27, and P29 of the 2.16-μ band of N2O and of the 5–6 line of the 1.66-μ band of CH4 have been measured in the spectrum of the low-sun observed from Mount Wilson. For both molecules, the rate of change of intensity with solar zenith angle is inconsistent with the existence of these gases in thin layers at altitudes of 15 km or greater. On the other hand, the observations satisfy very well the assumption of uniform mixing with the major constituents of the atmosphere.