ACETYLENE ON TITAN’S SURFACE
- Bear Fight Institute, 22 Fiddlers Rd, Winthrop, WA 98862 (United States)
- Laboratoire Astrophysique, Instrumentation et Modélisation (AIM), CNRS-UMR 7158, Université Paris-Diderot, CEA-SACLAY, F-91191 Gif sur Yvette (France)
- European Space Agency (ESA), European Space Astronomy Centre (ESAC), P.O. BOX 78, E-28691 Villanueva de la Caada, Madrid (Spain)
- Laboratoire de Planétologie et Géodynamique de Nantes, Université de Nantes, UMR 6112 CNRS, 2 rue de la Houssiniére BP92208, Nantes Cedex 3 (France)
- U.S. Geological Survey, Denver Federal Center, Denver, CO 80225 (United States)
Titan’s atmosphere is opaque in the near-infrared due to gaseous absorptions, mainly by methane, and scattering by aerosols, except in a few “transparency windows.” Thus, the composition of Titan’s surface remains difficult to access from space and is still poorly constrained. Photochemical models suggest that most of the organic compounds formed in the atmosphere are heavy enough to condense and build up at the surface in liquid and solid states over geological timescales. Acetylene (C{sub 2}H{sub 2}) net production in the atmosphere is predicted to be larger than any other compound and C{sub 2}H{sub 2} has been speculated to exist on the surface of Titan. C{sub 2}H{sub 2} was detected as a trace gas sublimated/evaporated from the surface using the Gas Chromatograph Mass Spectrometer after the landing of the Huygens probe. Here we show evidence of C{sub 2}H{sub 2} on the surface of Titan by detecting absorption bands at 1.55 and 4.93 μ m using the Cassini Visual and Infrared Mapping Spectrometer at three different equatorial areas—Tui Regio, eastern Shangri La, and Fensal–Aztlan/Quivira. We found that C{sub 2}H{sub 2} is preferentially detected in low-albedo areas, such as sand dunes and near the Huygens landing site. The specific location of the C{sub 2}H{sub 2} detections suggests that C{sub 2}H{sub 2} is mobilized by surface processes, such as surface weathering by liquids through dissolution/evaporation processes.
- OSTI ID:
- 22667715
- Journal Information:
- Astrophysical Journal, Vol. 828, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
Similar Records
COMPOSITIONAL SIMILARITIES AND DISTINCTIONS BETWEEN TITAN’S EVAPORITIC TERRAINS
THE {nu}{sub 8} BENDING MODE OF DIACETYLENE: FROM LABORATORY SPECTROSCOPY TO THE DETECTION OF {sup 13}C ISOTOPOLOGUES IN TITAN'S ATMOSPHERE