Chemical modelling of water deuteration in IRAS16293-2422

DOI DOI PDF 被引用文献4件 参考文献68件

書誌事項

公開日
2014-10-21
資源種別
journal article
DOI
  • 10.1093/mnras/stu1920
  • 10.48550/arxiv.1410.6366
公開者
Oxford University Press (OUP)

この論文をさがす

説明

IRAS 16293-2422 is a well studied low-mass protostar characterized by a strong level of deuterium fractionation. In the line of sight of the protostellar envelope, an additional absorption layer, rich in singly and doubly deuterated water has been discovered by a detailed multiline analysis of HDO. To model the chemistry in this source, the gas-grain chemical code Nautilus has been used with an extended deuterium network. For the protostellar envelope, we solve the chemical reaction network in infalling fluid parcels in a protostellar core model. For the foreground cloud, we explored several physical conditions (density, cosmic ionization rate, C/O ratio). The main results of the paper are that gas-phase abundances of H2O, HDO and D2O observed in the inner regions of IRAS16293-2422 are lower than those predicted by a 1D dynamical/chemical (hot corino) model in which the ices are fully evaporated. The abundance in the outer part of the envelope present chaotic profiles due to adsorption/evaporation competition, very different from the constant abundance assumed for the analysis of the observations. We also found that the large abundances of gas-phase H2O, HDO and D2O observed in the absorption layer are more likely explained by exothermic surface reactions rather than photodesorption processes.

20 pages, 15 figures. This version is slightly different from the published one because of language editor's modifications

収録刊行物

被引用文献 (4)*注記

もっと見る

参考文献 (68)*注記

もっと見る

関連プロジェクト

もっと見る

キーワード

詳細情報 詳細情報について

問題の指摘

ページトップへ