Titan's Stratospheric Haze Distribution Around The Equator

Details Titan's Stratospheric Haze Distribution Around The Equator Titan's Stratospheric Haze Distribution Around The Equator

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.2004d&link_type=abstract

American Astronomical Society, DPS meeting #40, #20.04; Bulletin of the American Astronomical Society, Vol. 40, p.422

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Scientific paper

Ever since the two Voyager spacecraft passed Titan in the early 1980's it is known that Titan exhibits a remarkable north-south asymmetry (NSA): one hemisphere is significantly darker (or lighter) than the other at a range of wavelengths, from ultraviolet to infrared. The most plausible interpretation for the NSA is a difference in stratospheric haze concentration between the two hemispheres.
We present a closer look at Titan's stratospheric haze distribution around the equator using Cassini's Composite Infrared Spectrometer (CIRS) and Visual and Infrared Mapping Spectrometer (VIMS). Six vertical profiles of haze extinction around 650 cm-1 between latitudes 20oS and 30oN and altitudes of 150 and 250 km are derived from CIRS limb data. These profiles confirm the distinct separation between the hemispheres as indicated by the shorter wavelength observations. VIMS and imaging data furthermore show an unexpected feature: a band close to the equator, which extends over a very narrow range of latitudes. The band possibly corresponds to a narrow region of increased haze opacity in the stratosphere. Further analysis of the VIMS data should yield more clues about this feature and implications for dynamical and/or chemical processes in Titan's equatorial atmosphere.

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