Titan H2O Clouds + ISS/UVIS

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Presentation transcript:

Titan H2O Clouds + ISS/UVIS Water in Titan's Atmosphere Image Cube Refinements Application to Enceladus Plume Locations Dione Example of co-analysis

Prediction of H2O Clouds Barth + Toon Model Predictions Based on UVIS temperature profile Maximum H2O abundance at 540 km N = 0.4 cm-3 H2O Particle size 0.01 microns

Data Sets Spica (Alpha Vir) and Shaula (Lambda Sco) occultations at T-B (December 13, 2004)

H2O Absorption Spectrum

Hydrocarbon Spectra CH4 C2H2 C2H4 C2H6 HCN

H20 Sensitivity

H2O Sensitivity with Hydrocarbons

Hints of H2O From Spica Occultation

H2O In Shaula Occultation

H2O Slopes Slope change at 1100 km Slope change at 900 km Slope between 1640Å and 1825Å Slope change at 1100 km Slope change at 900 km

Hydrocarbon analysis Correction of unattenuated spectrum with only hydrocarbons from Shemansky et al. occultation paper. At 550 km, log(nl) = CH4: 20.5 C2H2: 17.5 C2H4: 16.75 C2H6: 16.5 HCN: 17.25

Hydrocarbon Correction of Spica

Spica Correction

Spica Correction with H2O 530-550 km spectrum Hydrocarbon Model Hydrocarbon + Water

Shaula Occultation

Corrected Shaula Occultation 530-550 km spectrum Hydrocarbon Model Hydrocarbon + Water

Spatial Variability H2O clouds needed in northern hemisphere, but not southern. Future solar/stellar occultations should provide more tests.

Enceladus Image Cube Fountains of Enceladus (1688) November 27, 2005 Unknown time or distance Enceladus Plume Raw Preview (1701) November 27, 2005 170,600 km distance, 161º phase angle

Enceladus Plumes Based on relative size of moon in image and orbital geometry, image taken at 17:27:00 ± 5 minutes Plumes assumed to be limb aligned for mapping purposes.

Enceladus Plumes

Dione ISS/UVIS Analysis ISS Dione Raw Preview #1 (1564) October 11, 2005 ~09:50:00 UVIS ICYMAP003_PRIME Start Time - 14:43:28

Dione ISS Unwrap

Dione ISS/UVIS Pixels