Tests of stellar model atmospheres by optical interferometry: VLTI/VINCI limb-darkening measurements of the M4 giant psi phe

Details Tests of stellar model atmospheres by optical interferometry: VLTI/VINCI limb-darkening measurements of the M4 giant psi phe Tests of stellar model atmospheres by optical interferometry: VLTI/VINCI limb-darkening measurements of the M4 giant psi phe

2003-10-06

arxiv.org/abs/astro-ph/0310128v1

Astron.Astrophys. 413 (2004) 711-723

Astronomy and Astrophysics

Astrophysics

13 pages, 6 figures, accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20034149

We present K-band interferometric measurements of the limb-darkened intensity profile of the M4 giant star psi Phoenicis obtained with VLTI/VINCI. High-precision squared visibility amplitudes in the second lobe of the visibility function were obtained employing two 8.2 m UTs. This succeeded one month after light from UTs was first combined for interferometric fringes. In addition, we sampled the visibility function at small spatial frequencies using the 40cm test siderostats. Our measurement constrains the diameter of the star as well as its CLV. We construct a spherical hydrostatic PHOENIX model atmosphere based on spectrophotometric data from the literature and confront its CLV prediction with our interferometric measurement. We compare as well CLV predictions by plane-parallel hydrostatic PHOENIX, ATLAS9, and ATLAS12 models. We find that the Rosseland angular diameter as predicted by comparison of the spherical PHOENIX model with spectrophotometry is in good agreement with our interferometric diameter measurement. The shape of our measured visibility function in the second lobe is consistent with all considered PHOENIX and ATLAS model predictions, and significantly different from UD and FDD models. We derive high-precision fundamental parameters for psi Phe, namely a Rosseland angular diameter of 8.13 +/- 0.2 mas, with the Hipparcos parallax corresponding to a Rosseland linear radius R of 86 +/- 3 Rsun and an effective temperature of 3550 +/- 50 K, with R corresponding to a luminosity of log (L/Lsun)=3.02 +/- 0.06. Together with evolutionary models, these values are consistent with a mass of 1.3 +/- 0.2 Msun, and a surface gravity of log g = 0.68 +/- 0.11.

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