High-resolution 3-micron Spectral Features of Titan Identified with Updated CH3D and C2H6 Line Lists

Details High-resolution 3-micron Spectral Features of Titan Identified with Updated CH3D and C2H6 Line Lists High-resolution 3-micron Spectral Features of Titan Identified with Updated CH3D and C2H6 Line Lists

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.5610k&link_type=abstract

American Astronomical Society, DPS meeting #39, #56.10; Bulletin of the American Astronomical Society, Vol. 39, p.530

Astronomy and Astrophysics

Astrophysics

Scientific paper

We have re-analyzed the high-resolution spectra of Titan between 2.87 and 3.12 μm observed with the NIRSPEC/Keck II (Geballe et al. 2003, Astrophys. J. 583, L39) using updated CH3D (Nikitin et al. 2006, J. Mol. Spectrosc. 240, 14) and C2H6 lines including CH4, C2H2, and haze opacities. With the new synthetic spectra, we were able to identify all of the significant spectral features that were previously unidentified by Kim et al. (2005, Icarus, 173, 522), but they turned out to be due to weak lines of the above molecules, already detected species decades ago. Using an inversion radiative transfer program, we derived the opacities and reflectivities of haze particles as a function of altitude for the 2.87 - 2.92 μm wavelength range, where the atmosphere is partially transparent down to the surface. We also found that the haze layers become optically thick and the surface may not be seen easily at wavelengths in this range longer than 2.92 μm. Since the slit of the NIRSPEC covered the equatorial and temporal regions of Titan, our results are relevant to global averages excluding polar regions. We also discuss the possible enhancement of CH4 mixing ratios in the troposphere by investigating broad absorption wings of the CH3D lines assuming a globally constant CH3D/CH4 ratio; and we found that the possibility of the significant enhancement is very low.

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