Solving the mode identification problem in asteroseismology of F stars observed with Kepler

TL;DR

This paper addresses the challenge of mode identification in F-type stars' asteroseismology by using epsilon, effective temperature, and linewidths to distinguish correct oscillation modes in Kepler data.

Contribution

It introduces a method to resolve mode identification ambiguity in F stars by leveraging epsilon, effective temperature, and linewidths, applied to Kepler observations.

Findings

Successful identification of oscillation modes in F stars.

Epsilon values can be reliably deduced from temperature and linewidths.

Improved mode identification enhances asteroseismic analysis accuracy.

Abstract

Asteroseismology of F-type stars has been hindered by an ambiguity in identification of their oscillation modes. The regular mode pattern that makes this task trivial in cooler stars is masked by increased linewidths. The absolute mode frequencies, encapsulated in the asteroseismic variable epsilon, can help solve this impasse because the values of epsilon implied by the two possible mode identifications are distinct. We find that the correct epsilon can be deduced from the effective temperature and the linewidths and we apply these methods to a sample of solar-like oscillators observed with Kepler.