Dissociative recombination of H_2_D^+^ and the cosmic abundance of deuterium.

Details Dissociative recombination of H_2_D^+^ and the cosmic abundance of deuterium. Dissociative recombination of H_2_D^+^ and the cosmic abundance of deuterium.

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...309l...1l&link_type=abstract

Astronomy and Astrophysics, v.309, p.L1-L3

Astronomy and Astrophysics

Astrophysics

31

Atomic Data, Ism: Molecules, Ism: Abundances

Scientific paper

Deuterated molecules in interstellar clouds constitute a unique source of information on three interstellar parameters: the deuterium/hydrogen abundance ratio [D]/[H], the fractional ionisation in dense clouds, and the galactic ionizing flux (Dalgarno & Lepp 1984, Millar 1990). The molecular ion H_2_D^+^ plays a key role in the formation of deuterated molecules. Dissociative recombination with electrons is a major loss channel and a potential source of deuterium atoms. An ion storage ring has been used to obtain the total recombination rate coefficient, and the probabilities for decay into H+H+D, HD+H and H_2_+D. Using them in a model of the cloud L1529 we derive from observational data on HCO^+^ and DCO^+^ an upper limit to the fractional ionization of 2x10^-6^, a [D]/[H] ratio of 1.7x10^-5^ and an atomic D/H ratio of 2.7x10^-3^.

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