# Asteroseismology of main-sequence F stars with \textit{Kepler}: overcoming short mode lifetimes

## TL;DR

This paper demonstrates that unresolved blended mode centroids in F-type main-sequence stars can be effectively used for asteroseismology, providing accurate stellar parameters despite short mode lifetimes.

## Contribution

It introduces a method to perform asteroseismology using blended mode centroids instead of individual modes in F stars with short mode lifetimes.

## Key findings

- Centroid frequencies match results from individual mode analysis.
- Unresolved mode centroids yield comparable stellar parameters.
- Method extends asteroseismology to stars with overlapping modes.

## Abstract

Asteroseismology is a powerful way of determining stellar parameters and properties of stars like the Sun. However, main-sequence F-type stars exhibit short mode lifetimes relative to their oscillation frequency, resulting in overlapping radial and quadrupole modes. The goal of this paper is to use the blended modes for asteroseismology in place of the individual separable modes. We used a peak-bagging method to measure the centroids of radial-quadrupole pairs for 66 stars from the \textit{Kepler} LEGACY sample, as well as {\theta} Cyg, HD 49933, HD 181420, and Procyon. We used the relative quadrupole-mode visibility to estimate a theoretical centroid frequency from a grid of stellar oscillation models. The observed centroids were matched to the modelled centroids with empirical surface correction to calculate stellar parameters. We find that the stellar parameters returned using this approach agree with the results using individual mode frequencies for stars, where those are available. We conclude that the unresolved centroid frequencies can be used to perform asteroseismology with an accuracy similar to that based on individual mode frequencies.