Deuterium fractionation in the presolar nebula - Kinetic limitations on surface catalysis

Details Deuterium fractionation in the presolar nebula - Kinetic limitations on surface catalysis Deuterium fractionation in the presolar nebula - Kinetic limitations on surface catalysis

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987icar...72..430g&link_type=abstract

Icarus (ISSN 0019-1035), vol. 72, Nov. 1987, p. 430-436.

Physics

13

Catalytic Activity, Chemical Fractionation, Deuterium, Nebulae, Solar System, Nickel, Planetary Evolution, Stellar Evolution, Planets, Solar System, Deuterium, Fractionation, Solar Nebula, Kinetics, Thermal Effects, Equilibration, Abundance, Nickel, Time Scale, Chemistry, Isotopes, Hydrogen, Distribution, Formation, Origin, Abundance

Scientific paper

Models assuming low temperature equilibrium fractionation have previously been employed to explain the range of D/H values observed in the solar system and to make predictions of deuterium enhancement in the outer planets. While the reaction rates of the homogeneous partitioning reactions are prohibitively low at nebular temperatures, it has been suggested that catalysis on grains could shorten equilibration times sufficiently. This idea is quantitatively tested here. It is found that under highly idealized conditions - the full cosmic abundance of nickel available for catalysis in pure 5-μm grains - the equilibration time constant becomes greater than the lifetime of the nebula at temperatures lower than 560K. Even this firm lower limit is not cold enough to allow strong fractionation. Speculations are offered on alternative explanations for the distribution of hydrogen isotopes in the solar system.

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