New perspectives on Titan's upper atmosphere from a reanalysis of the Voyager 1 UVS solar occultations

By R. Vervack, B. Sandel, D. Strobel. 2004

174 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ecology

View Paper: https://www.semanticscholar.org/paper/9d29152b5c7fc2c82d67a02843a54807271bed8c

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In Astronomy and Astrophysics

1. J. Cui
2. V. Vuitton
3. V. Krasnopolsky
4. R. Yelle
5. M. McEwan
6. B. Bézard
7. Nicholas A. Teanby
8. A. Harri

In Ecology

1. R. Yelle
2. V. Krasnopolsky
3. M. McEwan
4. Remco J. de Kok
5. V. Vuitton
6. P. Irwin
7. J. Cui

Citations in the corpus

• The Nitrogen Chemistry of Titan’s Upper Atmosphere Revealed (2006, background): “For example, the HCN mole fraction decreases from ∼10 4 at 900 km (Vervack et al. 2004) to∼10 7 in the lower stratosphere (Flasar et al. 2005).”
• In situ measurements of the physical characteristics of Titan's environment (2005, background): “Several events are identified with triangles along the top axis: (1) stabilizer parachute opening, (2) mode change, (3) impulsive event in b, (4) surface touch down.”
• Ion chemistry and N-containing molecules in Titan's upper atmosphere (2007, methodology): “The mole fraction of HCN determined in our analysis (2 × 10−4) is in good agreement with the value inferred from the Voyager 1 solar occultation experiment, although obtained at 100 km lower altitude (Vervack et al., 2004).”
• Analysis of Titan's neutral upper atmosphere from Cassini Ion Neutral Mass Spectrometer measurements in the Closed Source Neutral mode (2009, methodology): “Previous results about the abundances of various neutral species in Titan’s thermosphere have also been obtained from the Voyager UVS solar occultation observations (Smith et al., 1982; Vervack et al., 2004).”
• Vertical abundance profiles of hydrocarbons in Titan's atmosphere at 15° S and 80° N retrieved from Cassini/CIRS spectra (2007, background): “Vervack et al. (2004) published a reanalysis of the Voyager 1 UVS solar occultations at latitudes of 4◦ N (ingress) and 16◦ S (egress).”
• A photochemical model of Titan's atmosphere and ionosphere (2009, methodology): “For the Voyager UVS occultations (Vervack et al., 2004), we compare the observed densities of a species with the N2 and CH4 densities from the model.”