Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared
H.C. Woodruff, M. Eberhardt, T. Driebe, K.-H. Hofmann, K. Ohnaka, A. Richichi, D. Schertl, M. Schoeller, M. Scholz, G. Weigelt, M. Wittkowski, and P.R. Wood
Astronomy and Astrophysics, v.421, p. 703-714(2004
We present K-band commissioning observations of the Mira star prototype o Cet obtained at the ESO Very Large Telescope Interferometer (VLTI) with the VINCI instrument and two siderostats. The observations were carried out between 2001 October and December, in 2002 January and December, and in 2003 January. Rosseland angular radii are derived from the measured visibilities by fitting theoretical visibility functions obtained from center-to-limb intensity variations (CLVs) of Mira star models. Using the derived Rosseland angular radii and the SEDs reconstructed from available photometric and spectrophotometric data, we find effective temperatures ranging from Teff = 3192 ± 200 K at phase Φ=0.13 to 2918 ± 183 K at Φ=0.26. Comparison of these Rosseland radii, effective temperatures, and the shape of the observed visibility functions with model predictions suggests that o Cet is a fundamental mode pulsator. Furthermore, we investigated the variation of visibility function and diameter with phase. The Rosseland angular diameter of o Cet increased from 28.9 ± 0.3 mas (corresponding to a Rosseland radius of 332 +- 38 R☉ for a distance of D=107 ± 12 pc) at Φ=0.13 to 34.9 ± 0.4 mas 402 ± 46 R☉ at Φ=0.4. The error of the Rosseland linear radius almost entirely results from the error of the parallax, since the error of the angular diameter is only approximately 1%.
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