Titan's atmospheric structure from Voyager 2 infrared spectra

Details Titan's atmospheric structure from Voyager 2 infrared spectra Titan's atmospheric structure from Voyager 2 infrared spectra

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993p%26ss...41..593l&link_type=abstract

Planetary and Space Science (ISSN 0032-0633), vol. 41, no. 8, p. 593-602

Astronomy and Astrophysics

Astronomy

15

Atmospheric Composition, Atmospheric Models, Carbon Compounds, Emission Spectra, Infrared Astronomy, Infrared Spectra, Satellite Atmospheres, Satellite Imagery, Titan, Abundance, Field Of View, Infrared Spectrometers, Signal To Noise Ratios, Spectral Signatures, Temperature Gradients, Voyager 2 Spacecraft

Scientific paper

Voyager 2 flew by Titan 9 months after Voyager 1 at a distance from its centre 100 times greater at closest approach (27 August 1981). A total of 115 infrared spectra are analysed here (taken mainly between 15 deg S and 60 deg N of latitude at emission angles less than 50 deg). The projected field of view of IRIS (the infrared spectrometer onboard) on Titan's disk is at best 60 deg, thus allowing for only two locally independent spectral selections. Our atmospheric model is applied on spectral averages covering the 200-1400/cm range (resolution = 4.3/cm). Molecules such as C2H2, C2H6, C3H4, C4H2, CH4, HCN and CO2 were clearly identified in emission with significant signal-to-noise ratios. Spectral features on the 3 sigma level appear at frequencies where C3H8 and C2H4 have signatures. No significant temporal variations within the 9 months were detected. Latitudinal variations exist both in temperature and composition. Our findings confirm previous analyses of Voyager 1 data and validate the associated atmospheric model.

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