Abstract
This paper presents a detailed and precise study of the characteristics of the Exoplanet Host Star and CoRoT main target HD 52265, as derived from asteroseismic studies. The results are compared with previous estimates, with a comprehensive summary and discussion. The basic method is similar to that previously used by the Toulouse group for solar-type stars. Models are computed with various initial chemical compositions and the computed p-mode frequencies are compared with the observed ones. All models include atomic diffusion and the importance of radiative accelerations is discussed. Several tests are used, including the usual frequency combinations and the fits of the \'echelle diagrams. The possible surface effects are introduced and discussed. Automatic codes are also used to find the best model for this star (SEEK, AMP) and their results are compared with that obtained with the detailed method. We find precise results for the mass, radius and age of this star, as well as its effective temperature and luminosity. We also give an estimate of the initial helium abundance. These results are important for the characterization of the star-planet system.
Highlights
In the past few years, the number of observed exoplanets has increased dramatically, owing to missions such as CoRoT (Baglin et al 2006) and Kepler (Koch et al 2010), as well as many other ground-based and space missions
Computations have been done for this star using the SEEK automatic code (Quirion et al 2010; Gizon et al 2012)
This code makes use of a large grid of stellar models computed with the Aarhus Stellar Evolution Code (ASTEC)
Summary
In the past few years, the number of observed exoplanets has increased dramatically, owing to missions such as CoRoT (Baglin et al 2006) and Kepler (Koch et al 2010), as well as many other ground-based and space missions (see the exoplanet encyclopedia for a complete summary). Constraints on the parameters and internal structure of the star can be obtained by comparing models with photometric and spectroscopic observations (Southworth 2011; Basu et al 2012), but the highest precision is obtained from asteroseismology, when the stellar oscillations may be observed and analyzed. An extensive study of the seismic rotation of HD 52265 was performed by Stahn (2011) and Gizon et al (2012) Spectroscopic observations of this star have been performed by several groups, who provide different values of the observed triplet ([Fe/H], log g, Teff).
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