The Deuterium to Hydrogen Ratio in the Atmospheres of Jupiter and Titan.

Details The Deuterium to Hydrogen Ratio in the Atmospheres of Jupiter and Titan. The Deuterium to Hydrogen Ratio in the Atmospheres of Jupiter and Titan.

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt........29k&link_type=abstract

Thesis (PH.D.)--STATE UNIVERSITY OF NEW YORK AT STONY BROOK, 1982.Source: Dissertation Abstracts International, Volume: 43-02,

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For determining the D/H ratios in the atmospheres of Titan and Jupiter, the 8.6 (mu)m band ((nu)(,6)) of CH(,3)D and the 7.7 (mu)m band ((nu)(,4)) of CH(,4) have been used. The (nu)(,6) band of CH(,3)D was observed in the laboratory at Stony Brook, and an absolute band intensity of 63.6 cm('-2)atm('-1) at 300 K and a constant hydrogen -broadened line width of 0.075 cm('-1)atm('-1) were obtained. Theoretical band models used for this thesis are also compiled. The accuracy of the random band models is improved by using real line strength distributions instead of the conventional simple models of line strength distributions. Several methods of saving computer time and improving accuracy in the line-by-line calculations are also discussed. The 8.6 (mu)m emission feature of Titan's infrared spectrum has been analyzed, using the Voyager temperature -pressure profile. Although both C(,3)H(,8) and CH(,3)D have bands at that wavelength, CH(,3)D turns out to be dominating the observed emission on Titan. A CH(,3)D/CH(,4) mixing ratio has been derived using these bands and the strong CH(,4) band at 7.7 (mu)m. The corresponding D/H ratio is. (DIAGRAM, TABLE OR GRAPHIC OMITTED...PLEASE SEE DAI). neglecting deuterium fractionation with other molecules. The main uncertainty in this value comes from the continuum emission characteristics. The D/H ratio is apparently significantly enhanced on Titan with respect to published values for Saturn. High resolution ((DELTA)(nu) = 1 cm('-1)) spectra of the 1100-1200 cm('-1) region of the central part of Jupiter have been analyzed. There is evidence for yearly variations in the tropospheric abundances of NH(,3), PH(,3), CH(,3)D and CH(,4). The best fit NH(,3) distribution curve shows a high mixing ratio NH(,3)/H(,2) = 3.3 (+OR-) 1.7 x 10('-4), below the 147 K layer (> 0.6 atmosphere). If NH(,3) ice particles are introduced as an opacity source, the NH(,3) mixing ratio below the 147 K layer can be lowered, but the fit is worse than the model excluding NH(,3) ice particles. The best fit PH(,3) distribution curve has a PH(,3)/H(,2) mixing ratio of 8.3 (+OR-) 2.0 x 10('-7) in the troposphere. A CH(,4)/H(,2) mixing ratio of 2.5 (+OR-) 0.4 x 10('-3) is found in the troposphere. The derived D/H ratio is. (DIAGRAM, TABLE OR GRAPHIC OMITTED...PLEASE SEE DAI). Most of the modeled flux in this spectral region comes from layer above the 170 K level (< 1 atmosphere).

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