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Mid-infrared interferometric observations of four oxygen-rich Mira variables

Published online by Cambridge University Press:  19 December 2013

I. Karovicova ,
M. Wittkowski ,
K. Ohnaka ,
D.A. Boboltz ,
E. Fossat  and
M. Scholz
I. Karovicova
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
M. Wittkowski
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
K. Ohnaka
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
D.A. Boboltz
Affiliation:
National Science Foundation, 4201 Wilson Boulevard, Arlington, VA, 22230, USA
E. Fossat
Affiliation:
Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d'Azur, 06300 Nice, France
M. Scholz
Affiliation:
Zentrum für Astronomie der Universität Heidelberg (ZAH), Institut für Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney NSW 2006, Australia
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Abstract

We present an investigation of the dust formation process in the atmospheres of the oxygen-rich AGB stars RR Aql, S Ori, GX Mon and R Cnc using spatially and spectrally resolved mid-infrared interferometric observations. We successfully compared multi epoch observations to a radiative transfer model of the dust shells, where the central stellar intensity profile is described by a series of dust-free dynamic model atmospheres based on self-excited pulsation models. We show that the Al2O3 shells have inner radii between 1.9 and 2.2 stellar photospheric radii, and that the silicate shells have inner radii between 4.1 and 4.6 stellar photospheric radii. The best-fit photospheric angular diameters are consistent with independent estimates. The model dust temperatures at the inner radii of 1.9–2.2 stellar radii and 4.1–4.6 stellar radii are consistent with dust condensation temperatures of Al2O3 and silicates, respectively.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 63: New Advances in Stellar Physics: From Microscopic to Macroscopic Processes , 2013 , pp. 191 - 196
Copyright
© EAS, EDP Sciences, 2013

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