Correcting stellar oscillation frequencies for near-surface effects

TL;DR

This paper develops an empirical correction method for near-surface effects in stellar oscillation frequencies, improving the accuracy of asteroseismic models by applying it to the Sun and other stars.

Contribution

It introduces a new empirical correction technique for near-surface frequency offsets, enhancing stellar modeling accuracy in asteroseismology.

Findings

Accurately estimates mean stellar densities.

Effective correction applied to multiple stars.

Improves agreement between observed and modeled frequencies.

Abstract

In helioseismology, there is a well-known offset between observed and computed oscillation frequencies. This offset is known to arise from improper modeling of the near-surface layers of the Sun, and a similar effect must occur for models of other stars. Such an effect impedes progress in asteroseismology, which involves comparing observed oscillation frequencies with those calculated from theoretical models. Here, we use data for the Sun to derive an empirical correction for the near-surface offset, which we then apply three other stars (alpha Cen A, alpha Cen B and beta Hyi). The method appears to give good results, in particular providing an accurate estimate of the mean density of each star.