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Session 91 - Structure of Molecular Clouds.
Oral session, Wednesday, January 15
Harbour A,
To better understand dense molecular cloud cores and to facilitate testing of existing chemical models, we have constructed a detailed model of these regions. In our model, we consider gas-phase chemistry (via the UMIST network), self-consistent dust continuum radiative transfer and dust temperature determination, and thermal balance of the gas (including gas-grain heating, and line cooling).
>From these data, we self-consistently solve the multi-level, NLTE line transfer problem including the dust continuum processes. The line transfer is solved for the species ^12C^16O, ^12C^18O, ^13C^16O, ortho-H_2^16O, ortho-H_2^18O, para-H_2^16O, amp; para-H_2^18O. In particular, we obtain water line strengths and profiles, which can be used for comparison with observations from SWAS and ISO.
We summarize some of our model results, with special attention to the capabilities and results of ISO and the upcoming SWAS mission. We note, in particular, that our model predicts water abundances that are consistent with those observed, and that CO should be the dominant gas coolant. Our model also suggests that the low lying water and CO transitions should have line strengths nearly independent of central luminosity, while the high-lying water transitions should be in absorption. Finally, like other recent models, we predict that OI 63 \mum emission may be quite strong.
The author(s) of this abstract have provided an email address for comments about the abstract: dotysd@rowland.pha.jhu.edu
