The diameter and evolutionary state of Procyon A. Multi-technique modeling using asteroseismic and i

  title={The diameter and evolutionary state of Procyon A. Multi-technique modeling using asteroseismic and i},
  author={Pierre Kervella and F. Th{\'e}venin and P. Morel and Gabrielle Berthomieu and Pascal J. Bord{\'e} and Janine Provost},
  journal={Astronomy and Astrophysics},
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 $\theta_{\rm UD} = 5.376\pm0.047$ mas and a limb darkened value of $\theta_{\rm LD} = 5.448\pm0.053$ mas. Together with the hipparcos parallax, this gives a linear diameter of $2.048\pm0.025$ $D_{\odot}$. We use this result in combination with spectroscopic, photometric… 

Figures and Tables from this paper

Modeling ofCen and Procyon using VLTI observations
We present a novel approach to model the nearby starsCen A & B and Procyon A using asteroseismic and interferometric constraints. Using the VINCI instrument installed at the VLT Interferometer
Models of Procyon A including seismic constraints
The nearby star Procyon is a visual binary containing the F5 IV-V subgiant Procyon A, orbited in a 40.84-year period by the faint DQZ white dwarf (WD) Procyon B. Using images obtained over two
The angular sizes of dwarf stars and subgiants Surface brightness relations calibrated by interferometry
The availability of a number of new interferometric measurements of Main Sequence and subgiant stars makes it possible to calibrate the surface brightness relations of these stars using exclusively
The radius and mass of the subgiant star β Hyi from interferometry and asteroseismology
We have used the Sydney University Stellar Interferometer to measure the angular diameter of β Hydri. This star is a nearby G2 subgiant the mean density of which was recently measured with high
The Procyon AB binary system (orbital period 40.838 yr, a newly refined determination) is near and bright enough that the component radii, effective temperatures, and luminosities are very well
An Astrometric Study of Procyon
We report on the analysis of observations of Procyon obtained with the Multichannel Astrometric Photometer during the years 1986-2004. While the results significantly increase the precision of the
On the Limb Darkening, Spectral Energy Distribution, and Temperature Structure of Procyon
We have fit synthetic visibilities from three-dimensional (CO5BOLD+PHOENIX) and one-dimensional (PHOENIX, ATLAS 12) model stellar atmospheres of Procyon (F5 IV) to high-precision interferometric data
Asteroseismology and evolutionary status of Procyon A
Models of Procyon A satisfying the actual observational constraints, particularly the asteroseismic ones, are discussed. The oscillations of these models were computed and analysed. We looked for
Limb Darkening: Getting Warmer
We present interferometric observations and model atmosphere analyses of three stars: the F-type subgiant Procyon, the A-type supergiant Deneb, and the B-type supergiant Rigel. We use VLTI/VINCI and


The diameters of $\alpha$ Centauri A and B - A comparison of the asteroseismic and VINCI/VLTI views
We compare the first direct angular diameter measurements obtained on our closest stellar neighbour, Centauri, to recent model diameters constrained by asteroseismic observations. Using the VINCI
A Redetermination of the Mass of Procyon
The parallax and astrometric orbit of Procyon have been redetermined from PDS measurements of over 250 photographic plates spanning 83 years, with roughly 600 exposures used in the solution. These
The interferometric diameter and internal structure of Sirius A
The interferometric observations of dwarf stars in the solar neighbourhood, combined with Hipparcos parallaxes provide very precise values of their linear diameters. In this paper, we report the
Signatures of Convection in the Spectrum of Procyon: Fundamental Parameters and Iron Abundance
We have observed the spectrum of Procyon A (F5 IV) from 4559 to 5780 Å with a signal-to-noise ratio of ~103 and a resolving power of 2 × 105. We have measured the line bisectors and relative line
Evolution and Seismology of Procyon
We have calculated an array of stellar models for Procyon A that are based on the best physics available to us, including the latest opacities and nuclear cross sections. The array of models spans
Procyon B: Outside the Iron Box
Procyon B is one of a select group of white dwarf stars in visual binaries that are used to put stringent constraints on the fundamental physics of stellar degeneracy. We present Space Telescope
Comparison of Stellar Angular Diameters from the NPOI, the Mark III Optical Interferometer, and the Infrared Flux Method
The Navy Prototype Optical Interferometer (NPOI) has been used to measure the angular diameters of 41 late-type giant and supergiant stars previously observed with the Mark III optical
Stellar Turbulent Convection: A New Model and Applications
Improvements of the mixing-length theory (MLT) of turbulent convection in stellar atmospheres are developed theoretically. It is pointed out that inaccuracies are introduced into MLT by the
Search for p-mode Frequencies on Procyon A
. Following the recent evidence for the presence of an excess of power around 1 mHz in the frequency spectrum of the Doppler shift measurements for Procyon (Martie et al., 1999), we searched for
Further improvements of a new model for turbulent convection in stars
The effects of including a variable molecular weight and of using the newest opacities of Rogers and Iglesias (1991) as inputs to a recent model by Canuto and Mazzitelli (1991) for stellar turbulent