Observations of D/H ratios in H2O, HCl, and HF on Venus and new DCl and DF line strengths

Intensities of the spectral lines in the fundamental bands of (DCl)-Cl-35 and DF were calculated using the semi-empirical dipole moment functions derived from the most accurate and precise measurements of intensities of the to-vibrational lines of (HCl)-Cl-35 and HF. Values obtained in this way for the deuterated species are superior to any available measured or calculated data to date. Our study of the D/H ratios in H2O, HCl, and HF on Venus is based on spatially-resolved high-resolution spectroscopy using the CSHELL spectrograph at NASA IRTF. Search for DF on Venus using its R5 (1-0) line at 3024.054 cm(-1) results in a DF mixing ratio of 0.23 +/- 0.11 ppb that corresponds to (D/H)(HF) = 420 +/- 200 times that in the Standard Mean Ocean Water (SMOW). H2O abundances on Venus were retrieved using lines at 3022.366 and 3025.761 cm(-1) that were observed at an exceptionally low overhead telluric water abundance of 03 pr. mm. The measured H2O mixing ratios at 74 km vary insignificantly between 55 degrees S and 55 degrees N with a mean value of 3.2 ppm. When compared with simultaneous observations of HDO near 2722 cm(-1), this results in (D/H)(H2O) = 95 +/- 15 times SMOW. Reanalysis of the observation of the (DCl)-Cl-35 R4 (1-0) line at 2141.540 cm(-1) (Krasnopolsky, V.A. [2012b]. Icarus 219, 244-249) using the improved line strength and more thorough averaging of the spectra gives (D/H)(HCI) = 190 +/- 50 times SMOW. The similarity of the measured (D/H)(H2O) = 95 +/- 15 at 74 km with 120 +/- 40 observed by De Bergh et al. (De Bergh, C., Bezard, B., Owen, T., Crisp, D., Maillard, J.P., Lutz, B.L. [1991]. Science 251, 547-549) below the clouds favors the constant (D/H)(H2O) from the surface to the mesosphere, in accord with the prediction by theory. D/H approximate to 100 removes a difference of a factor of 2 between H2O abundances in the observations by Krasnopolsky (Krasnopolsky, V.A. [2010b]. Icarus 209, 314-322) and the Venus Express nadir observations (Cottini, V., Ignatiev, Piccioni, G., Drossart, P., Grassi, D., Markiewicz, W.J. [2012]. Icarus 217, 561-569). Equivalent widths of the HDO and H2O lines are similar in our observations; therefore some errors cancel out in their ratios. Photochemistry of HCl in the mesosphere tends to enrich D in HCI and deplete it in H2O. This may be an explanation of the twofold difference between the observed D/H in HCl and H2O. An alternative explanation is based on (D/H)(H2O) approximate to 200 observed in the mesosphere by Bjoraker et al. (Bjoraker, G.L., Larson, H.P., Mumma, M.J., Timmermann, R., Montani, J.L. [1992]. Bull. Am. Astron. Soc. 24, 995) and Fedorova et al. (Fedorova, A. et al. J. Geophys. Res. 113, E00B22). This means an effective exchange of D between H2O and HCl and almost equal D/H in both species. However, this requires a twofold increase in D/H from the lower atmosphere to the mesosphere. This increase is not supported by theory; furthermore, condensation processes usually deplete D/H above the clouds. Photochemistry of HF has not been studied; it proceeds mostly in the lower thermosphere, and D/H in HF may be very different from that in H2O. Overall, the observational data on D/H in all hydrogen-bearing species on Venus are helpful to solve the problem of deuterium fractionation on Venus. (C) 2013 Elsevier Inc. All rights reserved.