A new seismic analysis of Alpha Centauri

@article{Thoul2003ANS,
  title={A new seismic analysis of Alpha Centauri},
  author={Anne Thoul and Richard Scuflaire and Arlette Noels and Benjamin Vatovez and Maryline Briquet and M-A. Dupret and Josefina Montalb{\'a}n},
  journal={Astronomy and Astrophysics},
  year={2003},
  volume={402},
  pages={293-297}
}
Models of α Cen A &Bh avebeen computed using the masses determined by Pourbaix et al. (2002) and the data derived from the spectroscopic analysis of Neuforge & Magain (1997). The seismological data obtained by Bouchy & Carrier (2001, 2002) do help improve our knowledge of the evolutionary status of the system. All the constraints are satisfied with a model which gives an age of about 6 Gyr for the binary. 

Figures and Tables from this paper

Models of α Centauri A and B with and without seismic constraints: time dependence of the mixing-length parameter

The a Centauri (a Cen) binary system is a well-known stellar system with very accurate observational constraints on the structure of its component stars. In addition to the classical non-seismic

Analysis of $\alpha$ Centauri AB including seismic constraints

Detailed models of α  Cen A and B based on new seismological data for α  Cen B by Carrier & Bourban ([CITE]) have been computed using the Geneva evolution code including atomic diffusion. Taking into

Core properties of α Centauri A using asteroseismology

Context. A set of long and nearly continuous observations of α Centauri A should allow us to derive an accurate set of asteroseismic constraints to compare to models, and make inferences on the

Asteroseismic Analysis of α Cen B: Preliminary Tests of Effects of Rotation and Interior Magnetic Field in the Solar-like Star

Taking into consideration the effects of rotation and interior magnetic field during the lifetime of the star, we reconstruct the model of a Cen B to satisfy the latest non-asteroseismic and

Classically and Asteroseismically Constrained 1D Stellar Evolution Models of α Centauri A and B Using Empirical Mixing Length Calibrations

The bright, nearby binary α Centauri provides an excellent laboratory for testing stellar evolution models, because it is one of the few stellar systems for which we have high-precision classical

Asteroseismology of $\mathsf{\alpha}$ Centauri A - Evidence of rotational splitting

Context. Asteroseismology provides a unique tool for studying stellar interiors. Recently p modes have been detected on the bright solar-like star α  Cen A thanks to high-precision radial-velocity

A Preliminary Seismic Analysis of 51 Pegasi: Large and Small Spacings from Standard Models

We present a preliminary theoretical seismic study of the astronomically famous star 51 Peg. This is done by first performing a detailed analysis within the Hertzsprung-Russell diagram (HRD). Using

Asteroseismology of the $\beta$ Cep star HD 129929 - II. Seismic constraints on core overshooting, internal rotation and stellar parameters

We perform a detailed seismic study of the β Cep star HD 129929. Our analysis is based on the recent derivation of six pulsation frequencies. These frequencies are unambiguously identified from the

The chemical composition of α Centauri AB revisited

  • T. Morel
  • Physics, Geology
    Astronomy & Astrophysics
  • 2018
The two solar-like stars α Cen A and B have long served as cornerstones for stellar physics in virtue of their immediate proximity, association in a visual binary, and masses that bracket that of the

Modeling epsilon Eri and Asteroseismic Tests of Element Diffusion

Taking into account the helium and metal diffusion, we explore the possible evolutionary status with a seismic analysis, of the MOST (Microvariability and Oscillations of STars) target: the star

References

SHOWING 1-10 OF 23 REFERENCES

Asteroseismology and calibration of alpha cen binary system

Using the oscillation frequencies of Cen A recently discovered by Bouchy & Carrier (2001, 2002), the available astrometric, photometric and spectroscopic data, we tried to improve the calibration of

Evolutionary models and the p-mode oscillation spectrum of Alpha Centauri A and B

Spectroscopically observed abundances of Furenlid and Meylan (1990) and Los Alamos Opacity Library opacities specifically constructed for this mixture are used to construct the most detailed models

Constraining the difference in convective blueshift between the components of alpha Centauri with precise radial velocities

New radial velocities of Cen A & B obtained in the framework the Anglo-Australian Planet Search programme as well as in the CORALIE programme are added to those by Endl et al. (2001) to improve the

Seismic Tests of the Sun's Interior Structure, Composition, and Age, and Implications for Solar Neutrinos

The structure of the deep interior of a variety of standard and nonstandard solar models constrained by the low-l p-mode oscillation data from GONG are presented. For standard models, we show that

α Centauri AB

Detailed models of α Centauri A and B based on the Hipparcos, Yale, and Söderhjelm parallaxes are compared. The consequences of the uncertainty in mass, luminosity, surface temperature, and

P-mode observations on Alpha Cen A

We have made a clear detection of p-mode oscillations in the nearest solar-like G2V star $\alpha$ Cen A with the CORALIE spectrograph on the 1.2-m Swiss telescope at the ESO La Silla Observatory. We

The acoustic spectrum of alpha Cen A

This paper presents the analysis of Doppler p-mode observations of the G2V star a Cen A obtained with the spectrograph CORALIE in May 2001. Thirteen nights of observations have made it possible to

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

Low-Temperature Rosseland Opacities

A new, comprehensive set of low-temperature opacity data has been assembled. From this basic data set, Rosseland and Planck mean opacities have been computed for temperatures between 12,500 and 700

Consistent Evolution of F Stars: Diffusion, Radiative Accelerations, and Abundance Anomalies

Consistent stellar evolution models of F stars (1.1-1.5 M☉) are calculated with radiative forces, opacities, and diffusion for all elements included in OPAL's opacity tables. The opacities and