Computer Science
Scientific paper
Mar 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980e%26psl..47...43n&link_type=abstract
Earth and Planetary Science Letters, vol. 47, no. 1, Mar. 1980, p. 43-50.
Computer Science
4
Ammonia, Planetary Nebulae, Planetology, Reaction Kinetics, Solar System, Hydrogen, Molecular Clouds, Nitrogen, Planetary Atmospheres, Protoplanets
Scientific paper
Kinetic model of ammonia formation by iron catalysis in the primordial solar nebula is developed. The maximum time to reach equilibrium concentration is determined for various temperatures between 1000 and 200 K on the basis of reaction rates derived from industrial data on iron catalysts for ammonia. Application of the method for calculating the equilibrium time to an arbitrary nebula cooling model which maximizes the time available for ammonia synthesis results in an upper limit of 3% of the equilibrium value to the proportion of nitrogen in the form of ammonia at the time of planetary accretion, with ammonia abundance decreasing with distance from the sun. It is concluded that kinetic rather than equilibrium considerations control the abundance of ammonia in the solar nebula, and implications of the dominance of nitrogen for the evolution of the atmospheres of the terrestrial and Jovian planets and the composition of comets are indicated.
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