2016A&A...596A..73B


Query : 2016A&A...596A..73B

2016A&A...596A..73B - Astronomy and Astrophysics, volume 596A, 73-73 (2016/12-1)

In-depth study of 16 Cyg B using inversion techniques.

BULDGEN G., SALMON S.J.A.J., REESE D.R. and DUPRET M.A.

Abstract (from CDS):

Context. The 16 Cyg binary system hosts the solar-like Kepler targets with the most stringent observational constraints. Indeed, we benefit from very high quality oscillation spectra, as well as spectroscopic and interferometric observations. Moreover, this system is particularly interesting since both stars are very similar in mass but the A component is orbited by a red dwarf, whereas the B component is orbited by a Jovian planet and thus could have formed a more complex planetary system. In our previous study, we showed that seismic inversions of integrated quantities could be used to constrain microscopic diffusion in the A component. In this study, we analyse the B component in the light of a more regularised inversion.
Aims. We wish to analyse independently the B component of the 16 Cyg binary system using the inversion of an indicator dedicated to analyse core conditions, denoted tu. Using this independent determination, we wish to analyse any differences between both stars due to the potential influence of planetary formation on stellar structure and/or their respective evolution.
Methods. First, we recall the observational constraints for 16 Cyg B and the method we used to generate reference stellar models of this star. We then describe how we improved the inversion and how this approach could be used for future targets with a sufficient number of observed frequencies. The inversion results were then used to analyse the differences between the A and B components.
Results. The inversion of the tu indicator for 16 Cyg B shows a disagreement with models including microscopic diffusion and sharing the chemical composition previously derived for 16 Cyg A. We show that small changes in chemical composition are insufficient to solve the problem but that extra mixing can account for the differences seen between both stars. We use a parametric approach to analyse the impact of extra mixing in the form of turbulent diffusion on the behaviour of the tu values. We conclude on the necessity of further investigations using models with a physically motivated implementation of extra mixing processes including additional constraints to further improve the accuracy with which the fundamental parameters of this system are determined.

Abstract Copyright: © ESO, 2016

Journal keyword(s): stars: interiors - stars: oscillations - stars: fundamental parameters - asteroseismology

Simbad objects: 2

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Number of rows : 2
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 52265 PM* 07 00 18.0357152121 -05 22 01.778490073   6.845 6.282     G0V 299 1
2 * 16 Cyg ** 19 41 49.09 +50 31 31.6           ~ 127 0

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2021.10.26-05:46:05

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