Circumstellar water vapour in M-type AGB stars: radiative transfer models, abundances, and predictions for HIFI

¹ Stockholm Observatory, AlbaNova University Center, 106 91 Stockholm, Sweden e-mail: maercker@astro.su.se
² Onsala Space Observatory, 439 92 Onsala, Sweden
³ European Southern Observatory, Casilla 19001, Santiago 19, Chile

Received: 15 September 2007
Accepted: 18 December 2007

Abstract

Context.Surprisingly high amounts of H₂O have recently been reported in the circumstellar envelope around the M-type asymptotic giant branch star W Hya. This has lead to the speculation that evaporation of icy cometary or planetary bodies might be an effective ongoing mechanism in such systems. However, substantial uncertainties remain, as the required radiative transfer modelling is difficult due to high optical depths, sub-thermal excitation and the sensitivity to the combined radiation field from the central star and dust grains.

Aims.By performing a detailed radiative transfer analysis, we determine fractional abundances of circumstellar H₂O in the envelopes around six M-type asymptotic giant branch stars. The models are also used to predict H₂O spectral line emission for the upcoming Herschel/HIFI mission.

Methods.We use Infrared Space Observatory Long Wavelength Spectrometer spectra to constrain the circumstellar fractional abundance distribution of ortho-H₂O, using a non-local thermal equilibrium, and non-local, radiative transfer code based on the accelerated lambda iteration formalism. The mass-loss rates and kinetic temperature structures for the sample stars are determined through radiative transfer modelling of CO line emission based on the Monte-Carlo method. The density and temperature profiles of the circumstellar dust grains are determined through spectral energy distribution modelling using the publicly available code Dusty.

Results.The determined ortho-H₂O abundances lie between 210^-4 and 1.510^-3 relative to H₂, with the exception of WX Psc, which has a much lower estimated ortho-H₂O abundance of only 210^-6, possibly indicating H₂O adsorption onto dust grains or recent mass-loss-rate modulations. The estimated abundances are uncertain by, at best, a factor of a few.

Conclusions.The high water abundance found for the majority of the sources suggests that either the “normal” chemical processes are very effective in producing H₂O, or else non-local thermal equilibrium atmospheric chemistry, grain surface reactions, or a release of H₂O (e.g. from icy bodies like Kuiper belt objects) play a role. However, more detailed information on the physical structure and the velocity field of the region where the water vapour lines are formed is required to improve abundance estimates. We provide predictions for ortho-H₂O lines in the spectral window of Herschel/HIFI. These spectrally resolved lines cover a wide range of excitation conditions and will provide valuable additional information on the physical and chemical properties of the inner stellar wind where H₂O is abundant.