Titan's haze through a brief period of time

Details Titan's haze through a brief period of time Titan's haze through a brief period of time

Apr 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010ttt..work...54b&link_type=abstract

Through Time; A Workshop On Titan's Past, Present and Future, NASA Goddard Space Flight Center, April 6th - 8th, 2010. Edited b

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Scientific paper

We investigate the time-variability of the appearance of Titan's haze at visible wavelengths from the visual channel (V) of Cassini's Visual and Infrared Mapping Spectrometer (VIMS) during the prime mission. After the Pioneer and Voyager flybys, semi-periodic Hubble Space Telescope (HST) monitoring since 1992 built up a low-spatial-resolution database of Titan's haze reflectivity over time. The VIMS-V dataset extends the haze monitoring baseline after the demise of HST's STIS instrument in 2003. In addition VIMS' many views per flyby lead to high signal-to-noise ratios, particularly when the data are binned by latitude. The high spatial resolution across Titan's disk allows us to accurately compare the morphological boundaries of haze features. VIMS' visual channel covers wavelengths between 0.35 and 1.03 microns, wider than the HST spectrograph wavelength range (0.53-0.96 microns). The spectra have sufficient spectral resolution to resolve methane absorption lines, which provide a proxy for altitude. While ground- and HST-based views are always at low phase angle, the VIMS-V phase angle varies by flyby. The phase provides complementary data, but also introduces a complicating factor when comparing the VIMS results with other datasets. The VIMS data show significant changes over Cassini's 4-year prime mission, sufficient to identify trends. Continued VIMS observations during the Cassini Solstice mission will extend the monitoring of these trends, outlining the haze changes over a full Titan season.

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