Continuous absorption cross sections of OH and CH have been computed for the temperature range 1000 K to 9000 K. Both OH and CH produce significant ultraviolet opacity in the sun and cool stars. CH... Show moreContinuous absorption cross sections of OH and CH have been computed for the temperature range 1000 K to 9000 K. Both OH and CH produce significant ultraviolet opacity in the sun and cool stars. CH is also significant in the visible at 400 nm. 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
