A Bayesian approach to the modelling of α Cen A

  title={A Bayesian approach to the modelling of $\alpha$ Cen A},
  author={Mich{\"a}el Bazot and S{\'e}bastien Bourguignon and J{\o}rgen Christensen-Dalsgaard},
  journal={Monthly Notices of the Royal Astronomical Society},
Determining the physical characteristics of a star is an inverse problem consisting of estimating the parameters of models for the stellar structure and evolution, and knowing certain observable quantities. We use a Bayesian approach to solve this problem for α Cen A, which allows us to incorporate prior information on the parameters to be estimated, in order to better constrain the problem. Our strategy is based on the use of a Markov chain Monte Carlo (MCMC) algorithm to estimate the… 

Figures and Tables from this paper


Understanding the physical conditions of dark molecular clouds and star-forming regions is an inverse problem subject to complicated chemistry that varies nonlinearly with both time and the physical

Bonnsai: a Bayesian tool for comparing stars with stellar evolution models

Powerful telescopes equipped with multi-fibre or integral field spectrographs combined with detailed models of stellar atmospheres and automated fitting techniques allow for the analysis of large

On the uncertain nature of the core of α Cen A

High-quality astrometric, spectroscopic, interferometric and, importantly, asteroseismic observations are available for $\alpha$ Cen A, which is the closest binary star system to earth. Taking all

Bayesian inference of stellar parameters based on 1D stellar models coupled with 3D envelopes

Stellar models utilizing 1D, heuristic theories of convection fail to adequately describe the energy transport in superadiabatic layers. The improper modelling leads to well-known discrepancies

On the impact of the structural surface effect on global stellar properties and asteroseismic analyses

In a series of papers, we have recently demonstrated that it is possible to construct stellar structure models that robustly mimic the stratification of multi-dimensional radiative

Benchmark ages for theGaiabenchmark stars

In the era of large-scale surveys of stars in the MilkyWay, stellar ages are crucial for studying the evolution of the Galaxy.But determining ages of field stars is notoriously difficult; therefore,

Stellar acoustic radii, mean densities and ages from seismic inversion techniques

Context. Determining stellar characteristics such as the radius, the mass or the age is crucial when studying stellar evolution, exoplanetary systems or characterising stellar populations in the

Tutorial: Asteroseismic Stellar Modelling with AIMS

The goal of aims (Asteroseismic Inference on a Massive Scale) is to estimate stellar parameters and credible intervals/error bars in a Bayesian manner from a set of asteroseismic frequency data and

Determining fundamental parameters of detached double-lined eclipsing binary systems via a statistically robust machine learning method

A new machine-learning approach to predict the modelling parameters for detached double-lined eclipsing binary systems, including the system age, based on observable quantities, which allows for the estimation of the importance of several physical effects which are included in a parametrized form in stellar models, such as convective core overshoot or stellar spot coverage.

A seismic and gravitationally bound double star observed by Kepler. Implication for the presence of a convective core

Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe stars using asteroseismology.Aims. The derivation of stellar



Bayesian peak-bagging of solar-like oscillators using MCMC: a comprehensive guide

Context. Asteroseismology has entered a new era with the advent of the NASA Kepler mission. Long and continuous photometric observations of unprecedented quality are now available which have

Bayesian Inference from Observations of Solar-like Oscillations

Stellar oscillations, which can be extracted from observed time series of the star's brightness or radial velocity, can provide a wealth of information about a star. In this paper we address the

Constraining fundamental stellar parameters using seismology. Application to α Centauri AB

We apply the Levenberg-Marquardt minimization algorithm to seismic and classical observables of theαCen binary system in order to derive the fundamental parameters ofαCenA+B, and to analyze the


Recent developments in instrumentation (e.g., in particular the Kepler and CoRoT satellites) provide a new opportunity to improve the models of stellar pulsations. Surface layers, rotation, and

Determination of stellar ages from isochrones: Bayesian estimation versus isochrone fitting

We present a new method, using Bayesian estimation, to determine stellar ages and their uncertainties from observational data and theoretical isochrones. The result for an individual star is obtained

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


Space-based projects are providing a wealth of high-quality asteroseismic data, including frequencies for a large number of stars showing solar-like oscillations. These data open the prospect for

Estimating the p-mode frequencies of the solar twin 18 Scorpii

Solar twins have been a focus of attention for more than a decade, because their structure is extremely close to that of the Sun. Today, thanks to high-precision spectrometers, it is possible to use

A Large Stellar Evolution Database for Population Synthesis Studies. I. Scaled Solar Models and Isochrones

We present a large and updated stellar evolution database for low-, intermediate-, and high-mass stars in a wide metallicity range, suitable for studying Galactic and extragalactic simple and

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