Thermal Structure of Titan's Atmosphere from Cassini Radio Occultations and Thermal- Infrared Spectra

Details Thermal Structure of Titan's Atmosphere from Cassini Radio Occultations and Thermal- Infrared Spectra Thermal Structure of Titan's Atmosphere from Cassini Radio Occultations and Thermal- Infrared Spectra

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p21b..02f&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P21B-02

Computer Science

Sound

0343 Planetary Atmospheres (5210, 5405, 5704), 6281 Titan

Scientific paper

The T12 and T14 flybys provided radio-occultation soundings in northern winter at four mid-latitude locations, three near 30 S and one near 50 S. The previous two occultation soundings from Voyager in northern spring were near the equator. In the lowest 20 km, the six retrieved temperature profiles from Cassini and Voyager are nearly identical, within a few tenths Kelvin of one another. An exception is the profile at 50 S, which is 1 K cooler than the others near the surface. Because of the proximity of the Cassini spacecraft to Titan during the T12 and T14 occultations, the soundings of the lowest 200 km of the atmosphere proceeded very quickly, typically over one to two minutes. As a result, stratospheric temperatures retrieved from the Cassini radio occultations are very sensitive to small timing uncertainties in the spacecraft trajectory, which can easily propagate to 10-20 K errors in temperature. Stratospheric temperatures retrieved from Cassini CIRS thermal- infrared spectra do not suffer from this difficulty, and they provide a means of eliminating these uncertainties. The high vertical resolution of the radio-occultation soundings complements the global-mapping capability of the CIRS data, and we provide examples illustrating the synergies.

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