High resolution solar spectra obtained from the ATMOS Fourier Transform Spectrometer (Spacelab 3 flight on April 29-May 6, 1985) have made it possible to identify and measure a large number of... Show moreHigh resolution solar spectra obtained from the ATMOS Fourier Transform Spectrometer (Spacelab 3 flight on April 29-May 6, 1985) have made it possible to identify and measure a large number of lines of the vibration-rotation fundamental bands of the X2 Pi state of CH. From about 100 lines of the 1-0, 2-1, and 3-2 bands and adopting theoretical transition probabilities, a solar carbon abundance of 8.60 + or - 0.05 is derived. This value is compared with new results inferred from other carbon abundance indicators. The final recommended solar abundance of carbon is 8.60 + or - 0.05. Show less
High resolution solar spectra obtained from the ATMOS Fourier Transform Spectrometer (Spacelab 3 flight on April 29 - May 6, 1985) made it possible to detect for the first time vibration-rotation... Show moreHigh resolution solar spectra obtained from the ATMOS Fourier Transform Spectrometer (Spacelab 3 flight on April 29 - May 6, 1985) made it possible to detect for the first time vibration-rotation lines of NH from the X3 Sigma(-) state near 3 microns. Using recent theoretical results for the transition probabilities of 23 selected measured lines of the 1-0 and 2-1 bands, a solar abundance of nitrogen of 8.06 + or - 0.07 is derived. This value is compared with the result derived from N I lines and agrees with the abundance obtained from the 3s-3p, 3p-3d and 3s-prime - 3p-prime transitions, A(N) = 8.00 + or - 0.09. The final recommended solar abundance of nitrogen is A(N) = 8.00 + or - 0.05. Show less
Grevesse, N.; Sauval, A.J.; Dishoeck, E.F. van 1984
High resolution solar spectra have permitted the measurement with great accuracy of equivalent widths of vibration-rotation lines of OH in the X2Pi state near 3-micron wavelength. Using recent... Show moreHigh resolution solar spectra have permitted the measurement with great accuracy of equivalent widths of vibration-rotation lines of OH in the X2Pi state near 3-micron wavelength. Using recent theoretical results for the transition probabilities, a solar oxygen abundance of (8.93 + or - 0.02) is derived which is in perfect agreement with the abundance deduced from the OH pure rotation lines. The solar abundance of oxygen is therefore A(O) = 8.92 + or - 0.035, as inferred from the analysis of 43 vibration-rotation lines and 81 pure rotation lines of the OH molecule. It is confirmed that the dipole moment function of Werner, Rosmus and Reinsch (1983) together with the Holweger-Mueller (1974) solar atmosphere model are to be preferred in the analysis of the data. Show less
