Deuterium chemistry in the Orion Bar

Details Deuterium chemistry in the Orion Bar Deuterium chemistry in the Orion Bar

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007msl..confe..12p&link_type=abstract

"Molecules in Space and Laboratory, meeting held in Paris, France, May 14-18, 2007. Editors: J.L. Lemaire, F. Combes. ISBN: 9782

Astronomy and Astrophysics

Astrophysics

Observations

Scientific paper

High levels of deuterium fractionation in gas-phase molecules are usually associated with cold regions, such as prestellar cores. High fractionation ratios are also observed in hot environments such as hot cores or hot corinos, where they are believed to be the result of evaporation of the icy mantles surrounding dust grains, and thus are remnants of a previous cold (either gas-phase or grain surface) chemistry. The recent detection of DCN towards the Orion Bar, in a clump at a characteristic temperature of ~70K, has shown that high deuterium fractionation can also be detected in PDRs, highlighting the possibility of forming deuterated molecules at a somewhat higher temperature. We present here the first results of observations aiming at studying in detail the chemistry at work in the Orion Bar PDR, to understand if DCN is produced by ice mantle evaporation, or is the result of warm gas-phase chemistry, involving the CH2D+ precursor ion, which survives higher temperatures than the usual H2D+ precursor.

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