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

被引:59
|
作者
Woodruff, HC
Eberhardt, M
Driebe, T
Hofmann, KH
Ohnaka, K
Richichi, A
Schertl, D
Schöller, M
Scholz, M
Weigelt, G
Wittkowski, M
Wood, PR
机构
[1] Max Planck Inst Radioastron, D-53121 Bonn, Germany
[2] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia
[3] Univ Sydney, Sch Phys, Inst Astron, Sydney, NSW 2006, Australia
[4] Heidelberg Univ, Inst Theoret Astrophys, D-69121 Heidelberg, Germany
[5] European So Observ, Santiago 19, Chile
[6] European So Observ, D-85748 Garching, Germany
关键词
instrumentation : interferometers; techniques : interferometric; stars : late-type; stars : AGB and post-AGB; stars : fundamental parameters; stars : individual : Mira;
D O I
10.1051/0004-6361:20035826
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 (Bessell et al. 1996; Hofmann et al. 1998; Tej et al. 2003b). Using the derived Rosseland angular radii and the SEDs reconstructed from available photometric and spectrophotometric data, we find effective temperatures ranging from T-eff = 3192 +/- 200 K at phase Phi = 0.13 to 2918 +/- 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 +/- 0.3 mas (corresponding to a Rosseland radius of 332 +/- 38 R-circle dot for a distance of D = 107 +/- 12 pc) at Phi = 0.13 to 34.9 +/- 0.4 mas (402 +/- 46 R-circle dot) 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%.
引用
收藏
页码:703 / 714
页数:12
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