Characterizing solar-type stars from full-length Kepler data sets using the Asteroseismic Modeling Portal

TL;DR

This study applies advanced asteroseismic modeling to Kepler data for 57 stars, revealing relationships between stellar properties and oscillation characteristics, and assessing the effectiveness of surface correction methods for solar-type stars.

Contribution

The paper demonstrates the application of the latest Asteroseismic Modeling Portal to a large stellar sample, uncovering new correlations and validating surface correction techniques for solar-like stars.

Findings

Variation of the mixing-length parameter with atmospheric properties.

Linear relation between stellar age and frequency separation ratio.

Empirical surface correction is effective for certain solar-type stars.

Abstract

The Kepler space telescope yielded unprecedented data for the study of solar-like oscillations in other stars. The large samples of multi-year observations posed an enormous data analysis challenge that has only recently been surmounted. Asteroseismic modeling has become more sophisticated over time, with better methods gradually developing alongside the extended observations and improved data analysis techniques. We apply the latest version of the Asteroseismic Modeling Portal (AMP) to the full-length Kepler data sets for 57 stars and the Sun, comprising planetary hosts, binaries, solar-analogs, and active stars. From an analysis of the derived stellar properties for the full sample, we identify a variation of the mixing-length parameter with atmospheric properties. We also derive a linear relation between the stellar age and a characteristic frequency separation ratio. In addition, we find that the empirical correction for surface effects suggested by Kjeldsen and coworkers is adequate for solar-type stars that are not much hotter (Teff < 6200 K) or significantly more evolved (logg > 4.2, <Delta_nu> > 80 muHz) than the Sun. Precise parallaxes from the Gaia mission and future observations from TESS and PLATO promise to improve the reliability of stellar properties derived from asteroseismology.