Volume 529, May 2011
|Number of page(s)||8|
|Published online||14 April 2011|
AMBER observations of the AGB star RS Capricorni: extended atmosphere and comparison with stellar models⋆
Dpt. Astronomia i Astrofísica, Universitat de València, C/ Dr. Moliner 50, 46100 Burjassot, Spain
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
3 Universität Heidelberg, Landessternwarte Königstuhl 12, 69117 Heidelberg, Germany
4 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
Received: 10 November 2010
Accepted: 29 January 2011
We report on K-band VLTI/AMBER observations at medium spectral resolution (~1500) of RS Capricorni, an M6/M7III semi-regular AGB star. From the spectrally dispersed visibilities, we measure the star diameter as a function of observing wavelength from 2.13 to 2.47 microns. We derive a Rosseland angular diameter of 7.95 ± 0.07 mas, which corresponds to an effective temperature of 3160 ± 160 K. We detect size variations of around 10% in the CO band heads, which are indicative of strong opacity effects of CO in the stellar photosphere. We also detect a linear increase in the size as a function of wavelength, beginning at 2.29 microns. Models of the stellar atmosphere, based on the mass of the star estimated from stellar-evolution models, predict CO-size effects of about half the sizes observed, and cannot reproduce the linear size increase with wavelength, redward of 2.29 microns. We are able to model this linear size increase with the addition of an extended water-vapor envelope around the star. However, we are unable to fit the data in the CO bandheads. Either the mass of the star is overestimated by the stellar-evolution models and/or there is an additional extended CO envelope in the outer part of the atmosphere. In any case, neither the water-vapor envelope nor the CO envelope can be explained using the current models.
Key words: techniques: interferometric / stars: atmospheres / stars: late-type / stars: invididual: RS Cap
© ESO, 2011
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