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We present K-band commissioning observations of the Mira star prototype o Cetobtained at the ESO Very Large Telescope Interferometer (VLTI) with the VINCIinstrument and two siderostats. The observations were carried out between 2001October and December, in 2002 January and December, and in 2003 January.Rosseland angular radii are derived from the measured visibilities by fittingtheoretical visibility functions obtained from center-to-limb intensityvariations (CLVs) of Mira star models (Bessel et al. 1996, Hofmann et al. 1998,Tej et al. 2003). Using the derived Rosseland angular radii and the SEDsreconstructed from available photometric and spectrophotometric data, we findeffective temperatures ranging from T_eff=3192 +/- 200 K at phase phi=0.13 to2918 +/- 183 K at phi=0.26. Comparison of these Rosseland radii, effectivetemperatures, and the shape of the observed visibility functions with modelpredictions suggests that o Cet is a fundamental mode pulsator. Furthermore, weinvestigated the variation of visibility function and diameter with phase. TheRosseland angular diameter of o Cet increased from 28.9 +/- 0.3 mas(corresponding to a Rosseland radius of 332 +/- 38 R_sun for a distance ofD=107 +/- 12 pc) at phi=0.13 to 34.9 +/- 0.4 mas (402 +/- 46 R_sun) at phi=0.4.The error of the Rosseland linear radius almost entirely results from the errorof the parallax, since the error of the angular diameter is only approximately1 %.Comment: 12 pages, 8 figures, accepted for publication in Astronomy &  Astrophysic

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