EDP Sciences
Free access
Issue
A&A
Volume 429, Number 3, January III 2005
Page(s) 1057 - 1067
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20041052


A&A 429, 1057-1067 (2005)
DOI: 10.1051/0004-6361:20041052

Mid-infrared interferometry of the Mira variable RR Sco with the VLTI MIDI instrument

K. Ohnaka1, J. Bergeat2, T. Driebe1, U. Graser3, K.-H. Hofmann1, R. Köhler3, Ch. Leinert3, B. Lopez4, F. Malbet5, S. Morel6, F. Paresce7, G. Perrin8, Th. Preibisch1, A. Richichi7, D. Schertl1, M. Schöller6, H. Sol8, G. Weigelt1 and M. Wittkowski7

1  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
    e-mail: kohnaka@mpifr-bonn.mpg.de
2  Observatoire de Lyon, 9 avenue Charles André, 69561 St.-Genis-Laval Cedex, France
3  Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
4  Observatoire de la Côte d'Azur, Département Fresnel, UMR 6528 CNRS, BP 4229, 06304 Nice Cedex 4, France
5  Laboratoire d'Astrophysique, Observatoire de Grenoble, 38041 Grenoble Cedex 9, France
6  European Southern Observatory, Casilla 19001, Santiago 19, Chile
7  European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
8  Observatoire de Paris-Meudon, 5 place Jules Janssen, 92190 Meudon, France

(Received 7 April 2004 / Accepted 8 September 2004)

Abstract
We present the results of the first mid-infrared interferometric observations of the Mira variable RR Sco with the MID-infrared Interferometer (MIDI) coupled to the European Southern Observatory's (ESO) Very Large Telescope Interferometer (VLTI), together with K-band observations using VLTI VINCI. The observations were carried out in June 2003, when the variability phase of the object was 0.6, using two unit telescopes (UT1 and UT3), as part of the Science Demonstration Time (SDT) program of the instrument. Projected baseline lengths ranged from 73 to 102 m, and a spectral resolution of 30 was employed in the observations, which enabled us to obtain the wavelength dependence of the visibility in the region between 8 and 13  $\mu$m. The uniform-disk diameter was found to be 18 mas between 8 and 10  $\mu$m, while it gradually increases at wavelengths longer than 10  $\mu$m to reach 24 mas at 13  $\mu$m. The uniform-disk diameter between 8 and 13  $\mu$m is significantly larger than the K-band uniform-disk diameter of 10.2  $\pm$ 0.5 mas measured using VLTI VINCI with projected baseline lengths of 15-16 m, three weeks after the MIDI observations. Our model calculations show that optically thick emission from a warm molecular envelope consisting of H 2O and SiO can cause the apparent mid-infrared diameter to be much larger than the continuum diameter. We find that the warm molecular envelope model extending to ~2.3  $R_{\star}$ with a temperature of ~1400 K and column densities of H 2O and SiO of 3  $\times$ 1021 cm -2 and 1  $\times$ 1020 cm -2, respectively, can reproduce the observed uniform-disk diameters between 8 and 10  $\mu$m. The observed increase of the uniform-disk diameter longward of 10  $\mu$m can be explained by an optically thin dust shell consisting of silicate and corundum grains. The inner radius of the optically thin dust shell is derived to be 7-8  $R_{\star}$ with a temperature of ~700 K, and the optical depth at 10  $\mu$m is found to be ~0.025.


Key words: infrared: stars -- techniques: interferometric -- stars: circumstellar matter -- stars: AGB and post-AGB -- stars: individual: RR Sco -- stars: mass-loss

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