Volume 404, Number 3, June IV 2003
|Page(s)||1087 - 1097|
|Section||Stellar structure and evolution|
|Published online||06 June 2003|
The diameters of α Centauri A and B
A comparison of the asteroseismic and VINCI/VLTI views
European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile
2 Département Cassini, UMR CNRS 6529, Observatoire de la Côte d'Azur, BP 4229, 06304 Nice Cedex 4, France
3 Observatoire de Genève, 1290 Sauverny, Switzerland
4 Département Fresnel, UMR CNRS 6528, Observatoire de la Côte d'Azur, BP 4229, 06304 Nice Cedex 4, France
Corresponding author: P. Kervella, email@example.com
Accepted: 9 April 2003
We compare the first direct angular diameter measurements obtained on our closest stellar neighbour, α Centauri, to recent model diameters constrained by asteroseismic observations. Using the VINCI instrument installed at ESO's VLT Interferometer (VLTI), the angular diameters of the two main components of the system, α Cen A and B, were measured with a relative precision of 0.2% and 0.6% respectively. Particular care has been taken in the calibration of these measurements, considering that VINCI is estimating the fringe visibility using a broadband K filter. We obtain uniform disk angular diameters for α Cen A and B of mas and mas, and limb darkened angular diameters of mas and mas. Combining these values with the parallax from Söderhjelm (1999), we derive linear diameters of and . These values are compatible with the masses published by Thévenin et al. (2002) for both stars.
Key words: techniques: interferometric / stars: binaries: visual / stars: evolution / stars: oscillations / stars: fundamental parameters / stars: individual: α Cen
© ESO, 2003
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