Primitive atmosphere and implications for the formation of channels on Mars

Details Primitive atmosphere and implications for the formation of channels on Mars Primitive atmosphere and implications for the formation of channels on Mars

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978natur.273..730y&link_type=abstract

Nature, vol. 273, June 29, 1978, p. 730-732.

Computer Science

6

Atmospheric Composition, Mars Atmosphere, Mars Surface, Photochemical Reactions, Alkanes, Atmospheric Models, Methane, Planetary Evolution, Solar Radiation, Ultraviolet Radiation, Mars, Flow, Surface, Atmosphere, Water, Methane, Hydrogen, Nitrogen, Alkanes, Thermal Properties, Hydrocarbons, Models, Channels

Scientific paper

It 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.

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