EDP Sciences
Free Access
Volume 424, Number 3, September IV 2004
Page(s) 1011 - 1024
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361:20041207

A&A 424, 1011-1024 (2004)
DOI: 10.1051/0004-6361:20041207

Warm water vapor envelope in Mira variables and its effects on the apparent size from the near-infrared to the mid-infrared

K. Ohnaka

Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
    e-mail: kohnaka@mpifr-bonn.mpg.de

(Received 30 April 2004 / Accepted 4 June 2004 )

We present a possible interpretation for the increase of the angular diameter of the Mira variables o Cet, R Leo, and $\chi$ Cyg from the K band to the 11  $\mu$m region revealed by the recent interferometric observations using narrow bandpasses where no salient spectral feature is present (Weiner et al. 2003a,b). A simple two-layer model consisting of hot and cool H 2O layers for the warm water vapor envelope, whose presence in Mira variables was revealed by previous spectroscopic observations, can reproduce the angular diameters observed with Infrared Spatial Interferometer as well as the high-resolution TEXES spectra obtained in the 11  $\mu$m region. The warm water vapor layers are optically thick in the lines, and therefore, strong absorption due to H 2O can be expected from such a dense water vapor envelope. However, the absorption lines are filled in by emission from the extended part of the envelope, and this results in the high-resolution 11  $\mu$m spectra which exhibit only weak, fine spectral features, masking the spectroscopic evidences of the dense, warm water vapor envelope. On the other hand, the presence of the warm water vapor envelope manifests itself as the larger angular diameters in the 11  $\mu$m region as compared to those measured in the near-infrared. Furthermore, comparison of the visibilities predicted in the near-infrared (1.5-3.8  $\mu$m) with observational results available in the literature demonstrates that our two-layer model for the warm water vapor envelope can also reproduce the observed near-infrared visibilities and angular diameters, and suggests that the wavelength dependence of the angular size of Mira variables in the infrared largely reflects the H 2O opacity. The radii of the hot H 2O layers in the three Mira variables are derived to be 1.5-1.7  $R_{\star}$ with temperatures of 1800-2000 K and H 2O column densities of (1-5)  $\times$ 1021 cm -2, while the radii of the cool H 2O layers are derived to be 2.2-2.5  $R_{\star}$ with temperatures of 1200-1400 K and H 2O column densities of (1-7)  $\times$ 1021 cm -2.

Key words: infrared: stars -- molecular processes -- techniques: interferometric -- stars: late-type -- stars: AGB and post-AGB -- stars: individual: o Cet, R Leo, $\chi$ Cyg

SIMBAD Objects

© ESO 2004

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