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arXiv · 1505.07696

H2O vapor excitation in dusty AGB envelopes. A PACS view of OH 127.8+0.0

R. Lombaert·L. Decin·A. de Koter·J. A. D. L. Blommaert·P. Royer·E. De Beck·B. L. de Vries·T. Khouri·M. Min
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Abstract

Context: AGB stars lose a large percentage of their mass in a dust-driven wind. This creates a circumstellar envelope, which can be studied through thermal dust emission and molecular emission lines. In the case of high mass-loss rates, this study is complicated by the high optical depths and the intricate coupling between gas and dust radiative transfer characteristics. An important aspect of the physics of gas-dust interactions is the strong influence of dust on the excitation of several molecules, including H2O. Aims: The dust and gas content of the envelope surrounding the high mass-loss rate OH/IR star OH 127.8+0.0, as traced by Herschel observations, is studied, with a focus on the H2O content and the dust-to-gas ratio. We report detecting a large number of H2O vapor emission lines up to J = 9 in the Herschel data, for which we present the measured line strengths. Methods: The treatments of both gas and dust species are combined using two numerical radiative transfer codes. The method is illustrated for both low and high mass-loss-rate sources. Specifically, we discuss different ways of assessing the dust-to-gas ratio: 1) from the dust thermal emission spectrum and the CO molecular gas line strengths; 2) from the momentum transfer from dust to gas and the measured gas terminal velocity; and 3) from the determination of the required amount of dust to reproduce H2O lines for a given H2O vapor abundance. These three diagnostics probe different zones of the outflow, for the first time allowing an investigation of a possible radial dependence of the dust-to-gas ratio. Results: ... Continued in article.

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R. Lombaert, L. Decin, A. de Koter, J. A. D. L. Blommaert, P. Royer, E. De Beck, B. L. de Vries, T. Khouri, M. Min. 2015-05-28. H2O vapor excitation in dusty AGB envelopes. A PACS view of OH 127.8+0.0. https://doi.org/10.1051/0004-6361%2F201218974

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