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Asteroseismic modelling of the Binary HD 176465
Benard Nsamba (Instituto de Astrofísica e Ciências do Espaço, U.Porto), M. J. P. F. G. Monteiro (Institute of Astronomy and Astrophysics, Portugal), T. L. Campante (School of Physics and Astronomy, University of Birmingham, UK)
The detection and analysis of oscillations in binary star systems is critical in understanding stellar structure and evolution. This is because such systems have the same initial chemical composition and age. Solar-like oscillations have been detected in both components of the asteroseismic binary HD 176465 by Kepler (White et al., 2016). This study presents an independent modelling of the two stars in this binary system. Stellar models generated using MESA (Modules for Experiment in Stellar Astrophysics) were fitted to both the observed individual frequencies and some spectroscopic parameters. The individual theoretical oscillation frequencies for the corresponding stellar models were obtained using GYRE as the pulsation code. A Bayesian approach was applied to find the Probability Distribution Functions of the stellar parameters using AIMS (Asteroseismic Inference on Massive Scale) as the optimization code. The age of the individual stars was found to agree with that obtained by White et al., (2016) of about 3.0 ± 0.5 Gyr old.