Deuterium fractionation in dense interstellar clouds

Details Deuterium fractionation in dense interstellar clouds Deuterium fractionation in dense interstellar clouds

May 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...340..906m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 340, May 15, 1989, p. 906-920. Research supported by SERC.

Astronomy and Astrophysics

Astrophysics

198

Chemical Fractionation, Deuterium, Interstellar Chemistry, Molecular Clouds, Orion Nebula, Abundance, Astronomical Models, Dissociation, Molecular Ions, Recombination Reactions, Time Dependence

Scientific paper

The time-dependent gas-phase chemistry of deuterium fractionation in dense interstellar clouds ranging in temperature between 10 and 70 K was investigated using a pseudo-time-dependent model similar to that of Brown and Rice (1986). The present approach, however, considers much more complex species, uses more deuterium fractionation reactions, and includes the use of new branching ratios for dissociative recombinations reactions. Results indicate that, in cold clouds, the major and most global source of deuterium fractionation is H2D(+) and ions derived from it, such as DCO(+) and H2DO(+). In warmer clouds, reactions of CH2D(+), C2HD(+), and associated species lead to significant fractionation even at 70 K, which is the assumed Orion temperature. The deuterium abundance ratios calculated at 10 K are consistent with those observed in TMC-1 for most species. However, a comparison between theory and observatiom for Orion, indicates that, for species in the ambient molecular cloud, the early-time results obtained with the old dissociative recombination branching ratios are superior if a temperature of 70 K is utilized.

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