Formation and Evolution of Titan’s Atmosphere

@article{Coustenis2005FormationAE,
  title={Formation and Evolution of Titan’s Atmosphere},
  author={A. Coustenis},
  journal={Space Science Reviews},
  year={2005},
  volume={116},
  pages={171-184}
}
The origin and evolution of Titan’s enigmatic atmosphere is reviewed. Starting with the present-day volatile inventory, the question of what was the original composition on Titan and how a satellite of similar size to other Galilean moons managed to acquire and hold on to the required material is discussed. In particular the possible sources and sinks of the main mother molecules (nitrogen, methane and oxygen) are investigated in view of the most recent models and laboratory experiments. The… Expand
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References

SHOWING 1-10 OF 50 REFERENCES
On the origin of Titan's atmosphere.
  • T. Owen
  • Chemistry, Medicine
  • Planetary and space science
  • 2000
TLDR
Titan's atmospheric methane appears to have been formed from carbon and other carbon compounds, either by gas phase reactions in the subnebula or by accretional heating during the formation of Titan. Expand
The composition and origin of Titan's atmosphere
Abstract The discovery that Titan had an atmosphere was made by the identification of methane in the satellite's spectrum in 1944. But the abundance of this gas and the identification of other majorExpand
Photochemically Driven Collapse of Titan's Atmosphere
TLDR
Radiative-convective and radiative-saturated equilibrium models of Titan's atmosphere show that methane depletion may have allowed Titan’s atmosphere to cool so that nitrogen, its main constituent, condenses onto the surface, collapsing Titan into a Triton-like frozen state with a thin atmosphere. Expand
D to H ratio and the origin and evolution of Titan's atmosphere
TLDR
Titan's atmosphere is enriched in deuterium by a factor of ≥3 relative to Jupiter and Saturn, and the greater part of the observed fractionation is probably derived from the formation of Titan and the subsequent evolution of Titan's atmosphere driven by photochemistry. Expand
An Evolutionary Turbulent Model of Saturn's Subnebula: Implications for the Origin of the Atmosphere of Titan
We have elaborated an evolutionary turbulent model of the subnebula of Saturn derived from that of Dubrulle (1993, Icarus 106, 59‐76) for the solar nebula, which is valid for a geometrically thinExpand
The D/H Ratio in Methane in Titan: Origin and History
Abstract We propose a new interpretation of the D/H ratio in CH4 observed in the atmosphere of Titan. Using a turbulent evolutionary model of the subnebula of Saturn (O. Mousis et al. 2002,Expand
Comets, impacts, and atmospheres.
TLDR
A mixture of three basic types of comets appears capable of accounting for the observed volatile inventories on Venus, Earth, and Mars, with the caveat that impact erosion is necessary to explain the present condition of the martian atmosphere. Expand
Evolution of CO on Titan
The early evolution of Titan's atmosphere is expected to produce enrichment in the heavy isotopomers of CO, ^(13)CO and C^(18)O, relative to ^(12)C^(16)O. However, the original isotopic signaturesExpand
Formation and Composition of Planetesimals
The composition of planetesimals depends upon the epoch and the location of their formation in the solar nebula. Meteorites produced in the hot inner nebula contain refractory compounds. VolatilesExpand
Monodeuterated methane in the outer solar system. III. Its abundance of Titan
The 3nv2 band of CH3D has been detected in spectra of Titan recorded at 1.6 microns with the Fourier transform spectrometer at the 4 m telescope of the Kitt Peak National Observatory. A value of theExpand
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