Asteroseismic modelling of the metal-poor star Tau Ceti

TL;DR

This study uses asteroseismology combined with non-asteroseismic data to accurately model the metal-poor star Tau Ceti, deriving its fundamental parameters and assessing observational methods.

Contribution

It presents a comprehensive asteroseismic modeling approach for Tau Ceti, integrating multiple data sources to determine its properties more reliably.

Findings

Optimal stellar models suggest Tau Ceti has a mass of 0.775-0.785 M☉ and an age of 8-10 Gyr.

Spectroscopic data provide more accurate stellar parameters than interferometric measurements.

The study demonstrates the effectiveness of combining asteroseismic and non-asteroseismic observations for stellar characterization.

Abstract

Context. Asteroseismology is an effcient tool not only for testing stellar structure and evolutionary theory but also constraining the parameters of stars for which solar-like oscillations are detected, presently. As an important southern asteroseismic target, Tau Ceti, is a metal-poor star. The main features of the oscillations and some frequencies of ? Ceti have been identified. Many scientists propose to comprehensively observe this star as part of the Stellar Observations Network Group. Aims. Our goal is to obtain the optimal model and reliable fundamental parameters for the metal-poor star Tau Ceti by combining all non-asteroseismic observations with these seismological data. Methods. Using the Yale stellar evolution code (YREC), a grid of stellar model candidates that fall within all the error boxes in the HR diagram have been constructed, and both the model frequencies and large- and small- frequency separations are calculated using the Guenther's stellar pulsation code. The \chi2c minimization is performed to identify the optimal modelling parameters that reproduce the observations within their errors. The frequency corrections of near-surface effects to the calculated frequencies using the empirical law, as proposed by Kjeldsen and coworkers, are applied to the models. Results. We derive optimal models, corresponding to masses of about 0.775 - 0.785 M? and ages of about 8 - 10 Gyr. Furthermore, we find that the quantities derived from the non-asteroseismic observations (effective temperature and luminosity) acquired spectroscopically are more accurate than those inferred from interferometry for ? Ceti, because our optimal models are in the error boxes B and C, which are derived from spectroscopy results.