Clouds, haze, and CH4, CH3D, HCN, and C2H2 in the atmosphere of Titan probed via 3 μm spectroscopy

Details Clouds, haze, and CH4, CH3D, HCN, and C2H2 in the atmosphere of Titan probed via 3 μm spectroscopy Clouds, haze, and CH4, CH3D, HCN, and C2H2 in the atmosphere of Titan probed via 3 μm spectroscopy

Feb 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005icar..173..522k&link_type=abstract

Icarus, Volume 173, Issue 2, p. 522-532.

Astronomy and Astrophysics

Astrophysics

15

Scientific paper

Using synthetic spectra derived from an updated model atmosphere together with a continuum model that includes contributions from haze, cloud and ground, we have re-analyzed the recently published (Geballe et al., 2003, Astrophys. J. 583, L39 L42) high-resolution 3 μm spectrum of Titan which contains newly-detected bands of HCN (in emission) and C2H2 and CH3D (in absorption), in addition to previously detected bands of CH4. In the 3.10 3.54 μm interval the analysis yields strong evidence for the existence of a cloud deck or optically thick haze layer at about the 10 mbar (˜ 100 km) level. The haze must extend well above this altitude in order to mask the strong CH4 lines at 3.20 3.50 μm. These cloud and haze components must be transparent at 2.87 2.92 μm, where analysis of the CH3D spectrum demonstrates that Titan's surface is glimpsed through a second cloud deck at about the 100 mbar (˜ 50 km) level. Through a combination of areal distribution and optical depth this cloud deck has an effective transmittance of ˜ 20%. The spectral shape of Titan's continuum indicates that the higher altitude cloud and haze particles responsible for suppressing the CH4 absorptions have a largely organic make-up. The rotational temperature of the HCN ranges from 140 to 180 K, indicating that the HCN emission occurs over a wide range of altitudes. This emission, remodeled using an improved collisional deactivation rate, implies mesospheric mixing ratio curves that are consistent with previously predictions. The stratospheric and mesospheric C2H2 mixing ratios are ˜10, considerably less than previous model predictions (Yung et al., 1984), but approximately consistent with recent observational results. Upper limits to mixing ratios of HC3N and C4H2 are derived from non-detections of those species near 3.0 μm.

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