NASA Logo

NTRS

NTRS - NASA Technical Reports Server

Back to Results
Chemistry and evolution of Titan's atmosphereThe chemistry and evolution of Titan's atmosphere are reviewed, in light of the scientific findings from the Voyager mission. It is argued that the present N2 atmosphere may be Titan's initial atmosphere, rather than one photochemically derived from an original NH3 atmosphere. The escape rate of hydrogen from Titan is controlled by photochemical production from hydrocarbons. CH4 is irreversibly converted to less hydrogen-rich hydrocarbons, which over geologic time accumulate on the surface to a layer thickness of about 0.5 km. Magnetospheric electrons interacting with Titan's exosphere may dissociate enough N2 into hot, escaping N atoms to remove about 0.2 of Titan's present atmosphere over geologic time. The energy dissipation of magnetospheric electrons exceeds solar EUV energy deposition in Titan's atmosphere by an order of magnitude, and is the principal driver of nitrogen photochemistry. The environmental conditions in Titan's upper atmosphere are favorable to building up complex molecules, particularly in the north polar cap region.
Document ID
19820060025
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Strobel, D. F.
(U.S. Navy, Naval Research Laboratory, Washington DC, United States)
Date Acquired
August 10, 2013
Publication Date
August 1, 1982
Subject Category
Lunar And Planetary Exploration
Accession Number
82A43560
Distribution Limits
Public
Copyright
Other

Available Downloads

There are no available downloads for this record.
No Preview Available