The complementary roles of interferometry and asteroseismology in determining the mass of solar-type stars

TL;DR

This paper investigates how combining interferometry and asteroseismology improves the accuracy of stellar parameter measurements, especially mass, for solar-type stars, highlighting the importance of independent radius measurements and seismic data.

Contribution

It provides quantitative analysis of the impact of radius measurements and seismic observables on stellar parameter determination, emphasizing the role of interferometry in reducing uncertainties.

Findings

Independent radius measurements can improve stellar mass accuracy to better than 2%.

Combining seismic data with radius measurements enhances parameter precision.

Measuring small frequency separation improves evolutionary stage and mixing-length estimates.

Abstract

How important is an independent diameter measurement for the determination of stellar parameters of solar-type stars? When coupled with seismic observables, how well can we determine the stellar mass? If we can determine the radius of the star to between 1% and 4%, how does this affect the theoretical uncertainties? Interferometry can provide an independent radius determination and it has been suggested that we should expect at least a 4% precision on such a measurement for nearby solar-type stars. This study aims to provide both qualitative and quantitive answers to these questions for a star such as our Sun, where seismic information will be available. We show that the importance of an independent radius measurement depends on the combination of observables available and the size of the measurement errors. It is important for determining all stellar parameters and in particular the mass, where a good radius measurement can even allow us to determine the mass with a precision better than 2%. Our results also show that measuring the small frequency separation significantly improves the determination of the evolutionary stage and the mixing-length parameter.