Titan’s aerosol and stratospheric ice opacities between 18 and 500 μm: Vertical and spectral characteristics from Cassini CIRS

• Published in: Icarus (New York, N.Y. 1962) N.Y. 1962), 2011-04, Vol.212 (2), p.762-778
• Main Authors: Anderson, Carrie M., Samuelson, Robert E.
• Format: Article
• Language: English
• Subjects: Aerosols; Altitude; Astronomy; Cassini mission; Earth, ocean, space; Exact sciences and technology; Ice clouds; Ices; Latitude; Radiative transfer; Solar system; Spectra; Stratosphere; Titan
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2011.01.024

► Titan’s aerosol spectrum (500 to 18 μm) does not change chemical composition between 15°N and 58°S. ► The aerosol has an emission feature at 140 cm −1, perhaps due to PAHs or nitrogenated aromatics. ► Strong evidence that stratospheric clouds composed of condensed trace organics extend globally. ► The broad stratospheric ice feature at ∼160 cm −1 is most likely blended HCN and HC 3N ices. ► The broad stratospheric ice feature derived near 80 cm −1 may be due to crystalline C 2H 6. Vertical distributions and spectral characteristics of Titan’s photochemical aerosol and stratospheric ices are determined between 20 and 560 cm −1 (500–18 μm) from the Cassini Composite Infrared Spectrometer (CIRS). Results are obtained for latitudes of 15°N, 15°S, and 58°S, where accurate temperature profiles can be independently determined. In addition, estimates of aerosol and ice abundances at 62°N relative to those at 15°S are derived. Aerosol abundances are comparable at the two latitudes, but stratospheric ices are ∼3 times more abundant at 62°N than at 15°S. Generally, nitrile ice clouds (probably HCN and HC 3N), as inferred from a composite emission feature at ∼160 cm −1, appear to be located over a narrow altitude range in the stratosphere centered at ∼90 km. Although most abundant at high northern latitudes, these nitrile ice clouds extend down through low latitudes and into mid southern latitudes, at least as far as 58°S. There is some evidence of a second ice cloud layer at ∼60 km altitude at 58°S associated with an emission feature at ∼80 cm −1. We speculate that the identify of this cloud may be due to C 2H 6 ice, which in the vapor phase is the most abundant hydrocarbon (next to CH 4) in the stratosphere of Titan. Unlike the highly restricted range of altitudes (50–100 km) associated with organic condensate clouds, Titan’s photochemical aerosol appears to be well-mixed from the surface to the top of the stratosphere near an altitude of 300 km, and the spectral shape does not appear to change between 15°N and 58°S latitude. The ratio of aerosol-to-gas scale heights range from 1.3–2.4 at about 160 km to 1.1–1.4 at 300 km, although there is considerable variability with latitude. The aerosol exhibits a very broad emission feature peaking at ∼140 cm −1. Due to its extreme breadth and low wavenumber, we speculate that this feature may be caused by low-energy vibrations of two-dimensional lattice structures of large molecules. Examples of such molecules include polyc