Cassini-Huygens/VIMS at T0 and Ta: A Taste of Titanic Things to Come K. H. Baines, B. Buratti, P. Drossart, C. Griffith, R. Jaumann, R. M. Nelson, R. H.

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Cassini-Huygens/VIMS at T0 and Ta: A Taste of Titanic Things to Come K. H. Baines, B. Buratti, P. Drossart, C. Griffith, R. Jaumann, R. M. Nelson, R. H. Brown, R. Clark, C. Sotin, T.Momary and the Cassini/VIMS Team

Salient Results from T0 Titan –Surface –Winds & Clouds –Emissions

Titan’s Surface Revealed at T0 -Crystal clear views of Titan’s surface achieved at several wavelengths in the near-infrared, particularly beyond 2.0 microns wavelength. -Variety of surface features observed -Evidence for variety of substances--including organic-based materials -No conclusive VIMS observational evidence yet for surface fluids -Specular reflection not observed on the approx. 2% of surface probed thus far

Observations at T0 Image HighRes in IR for some observations integration time between 160 ms and 640 ms. Phase angle : 65°

Cloud Distribution/Winds from T0 -Single major cloud feature near South Pole -88 degrees S. Latitude -~400 km diameter -Tracked for 12 hours -Several smaller, weaker clouds -Perhaps deeper cloudtops

Titan: Multiple South Polar Cloud Features

Cloud Structure Cloudtop: 20 ± 5 km Opacity: ~2 at 2  m Griffith Model

Titan Emissions Extensive atmosphere--10 times thicker than Earth’s-- Glows for hundreds of kilometers above surface Dayglow--Methane Fluorescence at 3.3 microns –Extended atmosphere ~ 1/3 of Titan’s radius Nightglow discovered=> warm stratosphere > 160 K –Generated by primarily by C0, C0 2 and CH 3 D

Nightside Emissions Altitude Profile

Titan Nightside 4.7-um Spectra CH 3 D CO 2 Blue: Average over the Night limb Red: Center of disk on nightside CO, likely Emission zone

CLOUD-TRACKED WINDS Latest Results For Major South-Pole Cloud Feature (8/31/04): 0.5 ± 3 m/s, prograde Based on: (1) Motions relative to surface features (2) Motions from C-Kernals Consistent with current theories of Titan’s winds

This Week at Titan…. Titan’s surface and atmosphere will be imaged up to 100 times higherspatial resolution than previously achieved.

VIMS will characterize the surface and atmosphere at the Huygens probe landing site.