期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 417, 期 4, 页码 2950-2961出版社
WILEY-BLACKWELL
DOI: 10.1111/j.1365-2966.2011.19455.x
关键词
astrochemistry; protoplanetary discs; circumstellar matter; stars: pre-main-sequence
资金
- Science and Technology Facilities Council of the United Kingdom (STFC)
- National Science Foundation [PHY05-51164]
- California Institute of Technology (Caltech)
- NASA [NNX08AK36G]
- Indiana University Institute for Advanced Study
- STFC
- NASA [NNX08AK36G, 100052] Funding Source: Federal RePORTER
- Science and Technology Facilities Council [ST/I001557/1, ST/F002092/1, ST/F006934/1] Funding Source: researchfish
- STFC [ST/F002092/1, ST/I001557/1, ST/F006934/1] Funding Source: UKRI
Until now, axisymmetric, a-disc models have been adopted for calculations of the chemical composition of protoplanetary discs. While this approach is reasonable for many discs, it is not appropriate when self-gravity is important. In this case, spiral waves and shocks cause temperature and density variations that affect the chemistry. We have adopted a dynamical model of a solar-mass star surrounded by a massive (0.39 M), self-gravitating disc, similar to those that may be found around Class 0 and early Class I protostars, in a study of disc chemistry. We find that for each of a number of species, e.g. H2O, adsorption and desorption dominate the changes in the gas-phase fractional abundance; because the desorption rates are very sensitive to temperature, maps of the emissions from such species should reveal the locations of shocks of varying strengths. The gas-phase fractional abundances of some other species, e.g. CS, are also affected by gas-phase reactions, particularly in warm shocked regions. We conclude that the dynamics of massive discs have a strong impact on how they appear when imaged in the emission lines of various molecular species.
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