Detection of Widespread Aromatic and Aliphatic Hydrocarbon Deposits on Titan's Surface Observed by VIMS and Excess Benzene observed in Titan's Thermosphere Observed by INMS

Details Detection of Widespread Aromatic and Aliphatic Hydrocarbon Deposits on Titan's Surface Observed by VIMS and Excess Benzene observed in Titan's Thermosphere Observed by INMS Detection of Widespread Aromatic and Aliphatic Hydrocarbon Deposits on Titan's Surface Observed by VIMS and Excess Benzene observed in Titan's Thermosphere Observed by INMS

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.4804c&link_type=abstract

American Astronomical Society, DPS meeting #38, #48.04; Bulletin of the American Astronomical Society, Vol. 38, p.574

Other

4

Scientific paper

Three previously unreported absorption features viewed through the 5-micron
spectral window of the atmosphere have been identified in Cassini Visual and Infrared Mapping Spectrometer (VIMS) spectra of Titan's surface. One of these absorptions(5.05 microns) matches the spectral position, width, and shape of solid benzene (C6H6), an aromatic hydrocarbon. The production of benzene and high-order nitriles in the Titan thermosphere has also been observed by the Cassini Ion and Neutral Mass Spectrometer (INMS). A second spectral feature at 4.97 microns appears to match simple alkanes, particularly solid or liquid methane and ethane, and possibly others as well. The third and weakest absorption at 5.02 microns is currently not identified, although solid acetonitrile (CH3CN) has a spectral band that is close to matching that of Titan, indicating that other nitriles might be candidates. All three absorption features are primarily associated with dark materials on the surface of Titan; benzene specifically maps in channels, "lakes," and boundaries of bright and dark terranes. Acetylene (C2H2), which is expected on Titan in higher abundances than benzene, has not been detected in surface deposits. Curiously, the benzene abundance on Titan's surface appears higher than predicted by current models of formation via photolysis products. One explanation for the apparently high benzene/acetylene ratio may be that the surface organics have been chemically processed more than previously considered. The concentrations of benzene observed by INMS also exceed model prediction by orders of magnitude. INMS has observed ion counterparts for these complex hydrocarbon and nitrile compounds, suggesting that ion neutral chemistry may play an important role in their production. The compounds formed in the thermosphere may be transported down into the stratosphere where they appear to complex in aerosol compounds before precipitating on the surface where they can be observed by VIMS.

Affiliated with

Also associated with

No associations

Rating

Detection of Widespread Aromatic and Aliphatic Hydrocarbon Deposits on Titan's Surface Observed by VIMS and Excess Benzene observed in Titan's Thermosphere Observed by INMS does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Detection of Widespread Aromatic and Aliphatic Hydrocarbon Deposits on Titan's Surface Observed by VIMS and Excess Benzene observed in Titan's Thermosphere Observed by INMS, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Detection of Widespread Aromatic and Aliphatic Hydrocarbon Deposits on Titan's Surface Observed by VIMS and Excess Benzene observed in Titan's Thermosphere Observed by INMS will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1001092