HCN in Titan Atmosphere by VIMS-IR Limb Observations

Details HCN in Titan Atmosphere by VIMS-IR Limb Observations HCN in Titan Atmosphere by VIMS-IR Limb Observations

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.2713a&link_type=abstract

American Astronomical Society, DPS meeting #38, #27.13; Bulletin of the American Astronomical Society, Vol. 38, p.529

Astronomy and Astrophysics

Astrophysics

Scientific paper

The HCN emission from the Titan atmosphere has already been observed by groundbased observations by the Keck II telescope at Mauna Kea in the Hawaii and reported by Geballe et al. (Astrophys.J., 583: L39-L42, 2003) and Kim et al. (Icarus, 173, 522-532, 2005) and also analyzed by a model for atmospheric fluorescence by Yelle and Griffith (Icarus, 166, 107-115, 2003).During the close encounter between Cassini and Titan which happened at the end of April 2006, the evidence of a weak emission from HCN around 3 micron has been identified in the limb observations of the Saturn's moon performed by the Visual and Infrared Mapping Spectrometer, VIMS, on board of the Cassini spacecraft. The atmospheric emission is measurable in a range of altitudes approximately between 100 and 500 km. Above the altitude of 500 km the atmospheric signal from the emission is probably too weak for being revealed by VIMS and it disappear in the background noise.

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