Mathematics – Logic
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p21a1325p&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #P21A-1325
Mathematics
Logic
0343 Planetary Atmospheres (5210, 5405, 5704), 0360 Radiation: Transmission And Scattering, 0644 Numerical Methods, 5470 Surface Materials And Properties, 6281 Titan
Scientific paper
The Cassini orbiter's Visual and Infrared Mapping Spectrometer (VIMS) observes Titan's surface intensity at wavelengths where its methane-rich atmosphere is heavily absorbing and light is strongly scattering. We aim to quantify the amount of I/F (spectral signal) from each component of Titan's atmosphere and surface, to aid analyses of Titan's surface that require use of the VIMS dataset (e.g., photoclinometry, geologic interpretation, spectral identification of surface materials, photometry). In a previous work (Pitman et al. 2008, LPSC XXXIX meeting), we presented radiative transfer model images of I/F for the entire disk of Titan, generated for Titan aerosol optical properties derived from Cassini-Huygens data and varying surface bidirectional reflectance functions at 9 wavelengths, 5 of which are VIMS methane windows. In this work, we combine gas absorber, aerosol, and surface signatures and subset these model I/F images for direct mapping and comparison to VIMS Titan data at different locations on Titan acquired at different observation times. Degrees of perturbation required in the Cassini-Huygens assumptions to match VIMS Titan data, comparison/contrast between results of spherical shell and plane-parallel radiative transfer methods, and single versus multiple scattering contributions of Titan's atmosphere at VIMS-relevant wavelengths will be discussed. Work performed under contract to NASA and under appointment to the NASA Postdoctoral Program (ORAU).
Baines Kevin Hays
Brown Harvey R.
Buratti Bonnie Jean
Dumont Philip J.
Pitman Karly M.
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