Tests of stellar model atmospheres by optical interferometry IV: VINCI interferometry and UVES spectroscopy of Menkar

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dc.creatorWittkowski, M.
dc.creatorAufdenberg, J. P.
dc.creatorDriebe, T.
dc.creatorRoccatagliata, V.
dc.creatorSzeifert, T.
dc.creatorWolff, B.
dc.date2006-10-05
dc.date.accessioned2026-07-07T10:23:47Z
dc.date.available2026-07-07T10:23:47Z
dc.descriptionWe present K-band interferometric and optical spectroscopic observations of Menkar obtained with the instruments VINCI and UVES at Paranal Observatory. Spherically symmetric PHOENIX stellar model atmospheres are constrained by comparison to our interferometric and spectroscopic data, and high-precision fundamental parameters of Menkar are obtained. Our high-precision VLTI/VINCI observations in the first and second lobes of the visibility function directly probe the model-predicted strength of the limb darkening effect in the K-band and the stellar angular diameter. The high spectral resolution of UVES allows us to confront observed and model-predicted profiles of atomic lines and molecular bands. We show that our derived PHOENIX model atmosphere for Menkar is consistent with both the measured strength of the limb-darkening in the near-infrared K-band and the profiles of spectral bands around selected atomic lines and TiO bandheads. At the detailed level of our high spectral resolution, however, noticeable discrepancies between observed and synthetic spectra exist. We obtain a Rosseland angular diameter of Theta_Ross=12.20 mas pm 0.04 mas. Together with the Hipparcos parallax, it corresponds to R_Ross=89 pm 5 R_sun, and together with the bolometric flux to T_eff=3795 K pm 70 K.Our approach illustrates the power of combining interferometry and high-resolution spectroscopy to constrain and calibrate stellar model atmospheres. The simultaneous agreement of the model atmosphere with our interferometric and spectroscopic data increases confidence in the reliability of the modelling of this star, while discrepancies at the detailed level of the high resolution spectra can be used to further improve the underlying model.
dc.description11 pages, 5 figures, accepted by A&A. Also available from http://www.aanda.org/articles/aa/pdf/forth/aa6032_06.pdf
dc.identifierhttps://arxiv.org/abs/astro-ph/0610150
dc.identifierhttp://arxiv.org/abs/astro-ph/0610150
dc.identifierAstron.Astrophys.460:855-864,2006
dc.identifierdoi:10.1051/0004-6361:20066032
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175959
dc.subjectAstrophysics
dc.titleTests of stellar model atmospheres by optical interferometry IV: VINCI interferometry and UVES spectroscopy of Menkar
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