Asteroseismology of main-sequence F stars with textit{Kepler}: overcoming short mode lifetimes. (arXiv:1902.05561v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Compton_D/0/1/0/all/0/1">Douglas L. Compton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bedding_T/0/1/0/all/0/1">Timothy R. Bedding</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stello_D/0/1/0/all/0/1">Dennis Stello</a>
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.
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.
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