Seasonal Changes In Saturn's Clouds

Details Seasonal Changes In Saturn's Clouds Seasonal Changes In Saturn's Clouds

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.4208c&link_type=abstract

American Astronomical Society, DPS meeting #40, #42.08; Bulletin of the American Astronomical Society, Vol. 40, p.474

Astronomy and Astrophysics

Astronomy

Scientific paper

Previous investigations indicate that Saturn's atmosphere consists of many hydrocarbons and trace chemical species such as methane (CH4), ammonia (NH3), and phosphine (PH3). NIR observations acquired from 1995 to 2006, equivalent to half a Saturnian year, are reduced and analyzed to study seasonal changes in the global distribution of these species in Saturn's clouds. The data was acquired from ground-based NASA/InfraRed Telescope Facility with NSFCAM and NSFCAM2 (1995-2006) and spacecraft Cassini/VIMS (2004-2006). Global cylindrical maps of reflectivitiy (or I/F) were created to extract latitudinal and pole-to-pole profiles of the planet's albedo. Since 1995, as Saturn's south pole received increasing solar insolation, the albedo maps (for wavelengths shorter than 3.0-microns) exhibit an increase in reflectivity at mid-latitudes in the southern hemisphere, decreasing towards the equator and the south pole. Our preliminary results indicate that at deeper levels in the atmosphere probed at 5.2-microns, Saturn's south pole is brightest, displaying trends opposite to those observed at shorter wavelengths. Baines et al. (2007, BAAS 38, 488) report north-south atmospheric asymmetry at 5-microns, based on Cassini/VIMS data. Data acquired from IRTF in February 2004 are consistent with Cassini/VIMS July 2004 data. We use this intersection of 2004 data sets as a benchmark to extend cloud models to the last ring plane crossing of 1995. We will apply Momary et al.'s (2007, BAAS 38, 487) cloud model to both IRTF and Cassini/VIMS data of 2004. Any difference between model and data will be quantified by adjusting the model input parameters to better match model output with observation. This project is pertinent for understanding the changing nature of Saturn;s clouds - differences in the opacity of different species, as Saturn approachs equinox in the near future. This project was supported by the NASA/Undergraduate Student Research Program (USRP) office.

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