Asteroseismic modelling of the Binary HD 176465

TL;DR

This paper presents detailed asteroseismic modeling of the binary star system HD 176465, utilizing Kepler data, stellar evolution models, and Bayesian analysis to determine the ages and properties of both stars.

Contribution

It provides an independent, comprehensive asteroseismic analysis of both components of HD 176465 using MESA, GYRE, and AIMS, confirming previous age estimates.

Findings

Ages of HD 176465 A and B are approximately 2.81 and 2.52 Gyr.

Models agree with previous asteroseismic and gyrochronology studies.

Demonstrates the effectiveness of Bayesian methods in stellar parameter estimation.

Abstract

The detection and analysis of oscillations in binary star systems is critical in understanding stellar structure and evolution. This is partly because such systems have the same initial chemical composition and age. Solar-like oscillations have been detected by Kepler in both components of the asteroseismic binary HD 176465. We present an independent modelling of each star in this binary system. Stellar models generated using MESA (Modules for Experiments in Stellar Astrophysics) were fitted to both the observed individual frequencies and complementary 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 a Massive Scale) as the optimisation code. The ages of HD 176465 A and HD 176465 B were found to be 2.81 $\pm$ 0.48 Gyr and 2.52 $\pm$ 0.80 Gyr, respectively. These results are in agreement when compared to previous studies carried out using other asteroseismic modelling techniques and gyrochronology.