Publications
of the
MPIfR Optical & Infrared Interferometry Group

Driebe, T., Ohnaka, K., Weigelt, G.

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

Cool Stars, Stellar Systems and the Sun
Annual Scientific Meeting of the Astronomische Gesellschaft, July 5-9, 2004, Hamburg, Germany

ESA Special Publications Series (ESA-SP), v.560, p.351-357 (2005)

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 the VLTI commissioning instrument 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. The projected baseline lengths ranged from 73 to 102m, and a spectral resolution of 30 was employed in the observations, which enabled us to obtain the wavelength 13μm. The uniform-disk diameter was found to be 18mas between 8 and 10μm, while it gradually increases at wavelengths longer than 10μm to reach 24mas at 13μm. The uniform-disk diameter between 8 and 13μm is significantly larger than the K-band uniform-disk diameter of 10.2 +- 0.5mas measured using VLTI VINCI with projected baseline lengths of 15-16m, three weeks after the MIDI observations. Our model calculations show that optically thick emission from a warm molecular envelope consisting of H₂O 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_* with a temperature of ~1400K and column densitites of H₂O and SiO of 3x10²¹cm^-2 and 1x10²⁰cm^-2, respectively, can reproduce the observed uniform-disk diameters between 8 and 10μm. The observed increase of the uniform-disk diameter longward of 10μm 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_* with a temperature of ~700K, and the optical depth at 10μm is found to be ~0.025.

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