Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sf2a.conf..266v&link_type=abstract
SF2A-2007: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics held in Grenoble, France, July
Astronomy and Astrophysics
Astrophysics
1
Scientific paper
Deuterium enhancement of monodeuterated species has been recognized for more than 30 years as a result of the chemical fractionation that results from the difference in zero point energies of deuterated and hydrogenated molecules. The key reaction is the deuteron exchange in the reaction between HD, the reservoir of deuterium in dark interstellar clouds, and the H3+ molecular ion, leading to the production of the H2D+ molecule, and the low temperature in dark interstellar clouds favors this production. Furthermore, the presence of multiply deuterated species have incited us (Phillips & Vastel 2003) to proceed further and consider the subsequent reaction of H2D+ with HD, leading to D2H+ (first detected by Vastel et al. 2004), which can further react with HD to produce D3+. In prestellar cores, where CO was found to be depleted (Bacmann et al. 2003), this production should be increased, as CO would normally destroy H3+. The first model including D2}H+ and D3}+ (Roberts, Herbst & Millar 2003) predicted that these molecules should be as abundant as H2D+. The first detection of the D2H+ was made possible by the recent laboratory measurement by Hirao & Amano (2003) for the frequency of the fundamental line of the para-D2H+. In this paper I present observations of H3D+ and D2H+ towards a sample of dark clouds and prestellar cores and show how the distribution of ortho-H2}D+ (11,0}-B11}) can trace the deuterium factory in prestellar cores. I will also present how future instrumentation will improve our knowledge concerning the deuterium enhancement of H3+.
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