The Process of Tholin Formation in Titan's Upper Atmosphere

By J. Waite, David T. Young, T. Cravens, A. Coates, F. Crary, B. Magee, J. Westlake. Science, 2007

626 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/427cc9f71ea4b6d929c410b2c1d48f5af8d8a900

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Jon Fortney
2. A. Showman
3. M. Marley
4. N. Madhusudhan
5. R. Freedman
6. D. Deming
7. T. Robinson
8. V. Parmentier

In Atmospheric Science

1. Jon Fortney
2. J. Cui
3. M. Marley
4. V. Vuitton
5. T. Robinson
6. P. Lavvas
7. R. Yelle
8. A. Showman

Citations in the corpus

• Formation and distribution of benzene on Titan (2008, neutral): “We base our estimate on the CH3 recombination rate of Wang et al. [2003], which was obtained from a combination of theoretical and experimental investigations down to 200 K.”
• Analysis of Titan's neutral upper atmosphere from Cassini Ion Neutral Mass Spectrometer measurements in the Closed Source Neutral mode (2009, methodology): “The INMS data obtained in the OSI mode have been presented recently by Cravens et al. (2006), Vuitton et al. (2007) and Waite et al. (2007) revealing that the composition of Titan’s ionosphere is very complex, with ∼50 ion species detected by the INMS.”
• Pale Orange Dots: The Impact of Organic Haze on the Habitability and Detectability of Earthlike Exoplanets (2016, background): “The Khare et al. (1984) optical constants were measured for Titan simulant hazes, but Archean-analog haze optical constants have only been measured at one wavelength (532 nm) in a previous study (Hasenkopf et al. 2010).”
• On the ionospheric structure of Titan (2009, background): “Moreover, Waite et al. (2007) obtained evidence for the formation of organic aerosols from simple molecules, which is shown to occur in the upper atmosphere, at altitudes around 1000 km.”
• Spectroscopy, morphometry, and photoclinometry of Titan's dunefields from Cassini/VIMS (2008, background): “Waite et al., 2007 ), the mechanism for generating 0.18–0.25 mm particles is not clear.”
• DISEQUILIBRIUM CARBON, OXYGEN, AND NITROGEN CHEMISTRY IN THE ATMOSPHERES OF HD 189733b AND HD 209458b (2011, background): “…could lead to the production of high-molecular-weight ions and photochemically produced aerosols through a Titan-like ion-chemistry process (e.g., Waite et al. 2007, 2009; Imanaka & Smith 2007; Vuitton et al. 2007, 2008), although it is also possible that the high abundance of H2O and/or CO and…”
• A photochemical model of Titan's atmosphere and ionosphere (2009, background): “The calculated profile of C2H4 perfectly fits the INMS data near 1000 km (Waite et al., 2007), the value from Vuitton et al. (2007) and the UVIS data below 1000 km, agrees with the Voyager UVS observations at 500–800 km and is close to the CIRS nadir value.”
• Negative ion chemistry in Titan's upper atmosphere (2008, background): “Various negative ions have been suggested as potential candidates for the low mass peaks observed by ELS (Coates et al., 2007a; Waite et al., 2007).”