Journal
ICARUS
Volume 199, Issue 2, Pages 449-457Publisher
ACADEMIC PRESS INC ELSEVIER SCIENCE
DOI: 10.1016/j.icarus.2008.09.017
Keywords
Titan; Atmospheres, composition; Spectroscopy; Infrared observations; Saturn; satellites
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Funding
- Korea Science and Engineering Foundation [R01-2008-00020002-0]
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We have reanalyzed the high-resolution spectrum of Titan between 2.87 and 3.12 mu m observed with NIRSPEC/Keck II on 2001 Nov. 21 in southern summer, using updated CH3D and C2H6 line-by-line models. From new synthetic spectra, we identify all but a few of the previously unidentified significant absorption spectral features in this wavelength range as due to these two species, both of which had been previously detected by Voyager and ground-based observations at other wavelengths. We also derive opacities and reflectivities of haze particles as functions of altitude for the 2.87-2.92 mu m wavelength range, where Titan's atmosphere is partially transparent down to the surface. The extinction per unit altitude is observed to increase from 100 km (similar to 8 mbar) toward lower altitude. The derived total optical depth is approximately 1.1 for the 2.97-2.92 mu m range. At wavelengths increasing beyond 2.92 mu m the haze layers become much more optically thick, and the surface is rapidly hidden from view. These conclusions apply to equatorial and southern-temperate regions on Titan, excluding polar regions. We also find it unlikely that there is a large enhancement of the tropospheric CH4 mole fraction over the Value reported from analysis of the Huygens/GCMS observations. (c) 2008 Elsevier Inc. All rights reserved.
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