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Modeling deuterium fractionation in cold and warm molecular environments with large chemical networks | | T. Albertsson
; D.A. Semenov
; Th. Henning
; | | Date: |
12 Oct 2011 | | Abstract: | Observations of deuterated species have long proven essential to probe
properties and thermal history of various astrophysical environments. We
present an elaborated chemical model that includes tens of thousands of
reactions with multi-deuterated species, both gas-phase and surface, in which
the most recent information on deuterium chemistry is implemented. A detailed
study of the chemical evolution under wide range of temperatures and densities
typical of cold molecular cores, warm protostellar envelopes, and hot
cores/corinos is performed. We consider two cases of initial abundances, with
1) mainly atomic composition and all deuterium locked in HD, and 2) molecular
abundances accumulated at 1 Myr of the evolution of a cold prestellar core. We
indicate deuterated species that are particularly sensitive to temperature
gradients and initial chemical composition. Many multiply-deuterated species
produced at 10 K by exothermic ion-molecule chemistry retain large abundances
even when temperature rises above 100 K, and can only be destroyed by
dissociation. Our model successfully explains observed D/H ratios of many
single, double, and triple-deuterated molecules, including water, methanol,
ammonia, and hydrocarbons in a variety of environments (cold cores, hot
protostellar envelopes and hot cores/corinos). We list the most abundant
deuterated species predicted by our model in different environments of low- and
high-mass star-formation regions, as well as key formation and destruction
pathways for DCO+, DCN and isotopologues of H2O, H3+ and CH3OH. | | Source: | arXiv, 1110.2644 | | Services: | Forum | Review | PDF | Favorites | |
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