The 3.4μm absorption in Titan’s stratosphere: Contribution of ethane, propane, butane and complex hydrogenated organics

@article{Cours2020The3A,
  title={The 3.4$\mu$m absorption in Titan’s stratosphere: Contribution of ethane, propane, butane and complex hydrogenated organics},
  author={T. Cours and D. Cordier and B. Seignovert and L. Maltagliati and L. Biennier},
  journal={Icarus},
  year={2020},
  volume={339},
  pages={113571}
}
Abstract The complex organic chemistry harbored by the atmosphere of Titan has been investigated in depth by Cassini observations. Among them, a series of solar occultations performed by the VIMS instrument throughout the 13 years of Cassini revealed a strong absorption centered at ∼ 3 . 4 μ m . Several molecules present in Titan’s atmosphere generate spectral features in that wavelength region, but their individual contributions are difficult to disentangle. In this work, we quantify the… Expand
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References

SHOWING 1-10 OF 84 REFERENCES
A photochemical model of Titan's atmosphere and ionosphere
Abstract The model for Titan by Krasnopolsky (2014, Icarus 236, 83-91) has been adjusted to Pluto's conditions during the New Horizons flyby. The model includes 419 reactions of 83 neutrals and 33… Expand
LARGE ABUNDANCES OF POLYCYCLIC AROMATIC HYDROCARBONS IN TITAN'S UPPER ATMOSPHERE
In this paper, we analyze the strong unidentified emission near 3.28 μm in Titan's upper daytime atmosphere recently discovered by Dinelli et al. We have studied it by using the NASA Ames PAH IR… Expand
Three-micron extinction of the Titan haze in the 250–700 km altitude range: Possible evidence of a particle-aging process
Context. The chemical nature of the Titan haze is poorly understood. The investigation carried out by the Cassini-Huygens suite of instruments is bringing new insights into this question. Aims. This… Expand
Retrieval and tentative indentification of the 3 μm spectral feature in Titan's haze
Recently, an unidentified 3.3–3.4 μm feature found in the solar occultation spectra of the atmosphere of Titan observed by Cassini/VIMS was tentatively attributed to the C–H stretching mode of… Expand
DETECTION OF PROPENE IN TITAN'S STRATOSPHERE
The Voyager 1 flyby of Titan in 1980 gave a first glimpse of the chemical complexity of Titan's atmosphere, detecting many new molecules with the infrared interferometer spectrometer (IRIS). These… Expand
Elusive anion growth in Titan’s atmosphere: Low temperature kinetics of the C3N− + HC3N reaction
Ion chemistry appears to be deeply involved in the formation of heavy molecules in the upper atmosphere of Titan. These large species form the seeds of the organic aerosols responsible for the opaque… Expand
The role of benzene photolysis in Titan haze formation
Abstract During the Cassini mission to the saturnian system, benzene (C 6 H 6 ) was observed throughout Titan’s atmosphere. Although present in trace amounts, benzene has been proposed to be an… Expand
The mesosphere and lower thermosphere of Titan revealed by Cassini/UVIS stellar occultations
Abstract Stellar occultations observed by the Cassini/UVIS instrument provide unique data that probe the mesosphere and lower thermosphere of Titan at altitudes between 400 and 1400 km. This region… Expand
Simulation of Titan’s atmospheric photochemistry - Formation of non-volatile residue from polar nitrile ices
We studied the photochemistry of frozen ice of a polar Titan’s atmospheric molecule cyanodiacetylene (HC5N) to determine the possible contribution of this compound to the lower altitude… Expand
Photochemical activity of Titan's low-altitude condensed haze.
TLDR
It is demonstrated that indeed tholin-like haze formation could occur on condensed aerosols throughout the atmospheric column of Titan, and C4N2 ices undergo condensed-phase photopolymerization (tholin formation) at wavelengths as long as 355 nm pertinent to solar radiation reaching a large portion of Titan's atmosphere. Expand
...
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5
...