Volume 413, Number 1, January I 2004
|Page(s)||251 - 256|
|Section||Stellar structure and evolution|
|Published online||17 December 2003|
The diameter and evolutionary state of Procyon A
Multi-technique modeling using asteroseismic and interferometric constraints
European Southern Observatory, Casilla 19001, Vitacura, Santiago 19, Chile
2 Département Cassini, UMR CNRS 6529, Observatoire de la Côte d'Azur, BP 4229, 06304 Nice Cedex 4, France
3 LESIA, Observatoire de Paris-Meudon, 5, place Jules Janssen, 92195 Meudon Cedex, France
Corresponding author: P. Kervella, Pierre.Kervella@eso.org
Accepted: 20 August 2003
We report the angular diameter measurement obtained with the VINCI/VLTI instrument on the nearby star Procyon A (α CMi A, F5IV–V), at a relative precision of ±0.9%. We obtain a uniform disk angular diameter in the K band of mas and a limb darkened value of mas. Together with the hipparcos parallax, this gives a linear diameter of . We use this result in combination with spectroscopic, photometric and asteroseismic constraints to model this star with the CESAM code. One set of modeling parameters that reproduces the observations within their error bars are an age of 2314 Myr, an initial helium mass fraction and an initial mass ratio of heavy elements to hydrogen . We also computed the adiabatic oscillation spectrum of our model of Procyon A, giving a mean large frequency separation of Hz. This value is in agreement with the seismic observations by Martić et al. ([CITE], [CITE]). The interferometric diameter and the asteroseismic large frequency spacing together suggest a mass closer to 1.4 than to 1.5 . We conclude that Procyon is currently ending its life on the main sequence, as its luminosity class indicates.
Key words: stars: individual: α CMi / stars: fundamental parameters / stars: evolution / techniques: interferometric
© ESO, 2004
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