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Primitive atmosphere and implications for the formation of channels on MarsIt is suggested that, if primitive Mars had a reducing atmosphere composed mainly of methane, this atmosphere could be polymerized by solar ultraviolet radiation to produce higher hydrocarbons. These compounds, which would be low-viscosity liquids at present temperatures on Mars, could have contributed to the formation of channels. The Martian atmosphere model used in the analysis is similar to Sagan's (1977), except that ammonia is omitted. Major reactions in this early Martian atmosphere are examined, and the number densities of the lighter alkanes in the lower atmosphere of Mars are determined. Since the photochemical mechanism investigated here would provide only a modest amount of fluid for a comparatively brief period of time (10-100 million years), liquid alkanes would not be the major factor in the formation of the channels, although their derivatives could contribute to the greenhouse effect or depress the freezing point of water.
Document ID
19780058551
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Yung, Y. L.
(California Institute of Technology Pasadena, Calif., United States)
Pinto, J. P.
(NASA Goddard Institute for Space Studies New York, N.Y., United States)
Date Acquired
August 9, 2013
Publication Date
June 29, 1978
Publication Information
Publication: Nature
Volume: 273
Subject Category
Lunar And Planetary Exploration
Accession Number
78A42460
Funding Number(s)
CONTRACT_GRANT: NSG-2283
CONTRACT_GRANT: NSG-5163
Distribution Limits
Public
Copyright
Other

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