Distribution of molecular hydrogen in the atmosphere of Titan

Details Distribution of molecular hydrogen in the atmosphere of Titan Distribution of molecular hydrogen in the atmosphere of Titan

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983jgr....88.8716b&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 88, Nov. 1, 1983, p. 8716-8720.

Astronomy and Astrophysics

Astronomy

16

Atmospheric Composition, Hydrogen, Molecular Diffusion, Satellite Atmospheres, Titan, Gas Temperature, Planetology, Spaceborne Astronomy, Vertical Distribution, Voyager 1 Spacecraft

Scientific paper

The diffusion problem of light gases in the atmosphere of Titan is reassessed after Voyager encounter. The pre-Voyager theoretical work of Hunten (1973) is completed by the use of parameters derived from Voyager encounter: the radial distances of turbopause level (3500 km) and critical level (4100 km), the exospheric temperature (186 K) and the volume mixing ratio of 0.002 for H2. An analytical expression of the solution of the diffusion equation is given for a spherical geometry and an isothermal atmosphere. It is used to predict an altitude profile of H2 in the upper atmosphere of Titan. The modification of this profile by a possible return flow of H2 from a torus to the atmosphere of Titan is addressed and is found negligible since there is observational evidence from Voyager that the H2 density is less than 100/cu cm in the torus, at large distance from Titan. The H2 concentration at the exobase level is 310,000/cu cm, and the thermal escape of H2 is nearly equal to the diffusion limiting flux of 3.4 x 10 to the 9th molecules/sq cm sec at the turbopause level. Photodissociation of CH4 has to provide for an equal constant supply of H2.

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