• DOI:10.1051/0004-6361:20035826
• Corpus ID: 17009595

Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared

@article{Woodruff2004InterferometricOO,
  title={Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared},
  author={H. Woodruff and Maren Eberhardt and Thomas Driebe and K. H. Hofmann and Keiichi Ohnaka and A Richichi and Dieter Schertl and Markus Schoeller and Miklas Scholz and Gerd Weigelt and Markus Wittkowski and P. R. Wood Max Planck Institute for Radioastronomy and Bonn and European Southern Observatory and Institute of Theoretical Astrophysics and University of Heidelberg and Institute of Radio Astronomy and School of Cosmic Physics and University of Western Sydney and Research School of Astronomy and Astrophysics and Australian Nat. Univ. and Weston Creek},
  journal={Astronomy and Astrophysics},
  year={2004},
  volume={421},
  pages={703-714}
}

• H. Woodruff, M. Eberhardt, +20 authors Weston Creek
• Published 13 April 2004
• Physics
• Astronomy and Astrophysics

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 [CITE]. Using the derived Rosseland angular radii and the SEDs reconstructed from available photometric and spectrophotometric data, we find effective temperatures ranging from $T_{\rm eff}=3192 \pm 200$ K at phase $\Phi=0.13$ to $2918 \pm 183$ K at $\Phi=0.26$. 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 $28.9 \pm 0.3$ mas (corresponding to a Rosseland radius of $332 \pm 38~R_{\odot}$ for a distance of $D=107\pm12~{\rm pc}$) at $\Phi=0.13$ to $34.9 \pm 0.4$ mas ($402 \pm 46~R_{\odot}$) at $\Phi=0.4$. 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%.