Asteroseismic analysis of 15 solar-like oscillating evolved stars
2021
Asteroseismology using space-based telescopes is vital to our understanding
of stellar structure and evolution. {\textit{CoRoT}}, {\textit{Kepler}}, and
{\textit{TESS}} space telescopes have detected large numbers of solar-like
oscillating evolved stars. %(kaynaklar, Kallinger, vb ). Solar-like oscillation
frequencies have an important role in the determination of fundamental stellar
parameters; in the literature, the relations between the two is established by
the so-called scaling relations. % These scaling relations are in better
agreement with mass and radius of main-sequence stars with large separation
($\Delta\nu$) and frequency of maximum amplitude (${\nu_{\rm max}}$). In this
study, we analyse data obtained from the observation of 15 evolved solar-like
oscillating stars using the {\textit{Kepler}} and ground-based %\textit{CoRoT}
telescopes. The main purpose of the study is to determine very precisely the fundamental
parameters of evolved stars by constructing interior models using asteroseismic
parameters. We also fit the reference frequencies of models to the
observational reference frequencies caused by the He {\scriptsize II}
ionization zone. The 15 evolved stars are found to have masses and radii within ranges of
$0.79$-$1.47$ $M_{\rm sun}$ and $1.60$-$3.15$ $R_{\rm sun}$, respectively.
Their model ages range from $2.19$ to $12.75$ Gyr. %Using a number of methods
based on conventional and modified scaling relations and evolutionary models
constructed with using the {\small {MESA}} code, we determine stellar radii,
masses and ages. It is revealed that fitting reference frequencies typically
increase the accuracy of asteroseismic radius, mass, and age. The typical
uncertainties of mass and radius are $\sim$ 3-6 and $\sim$ 1-2 per cent,
respectively. Accordingly, the differences between the model and literature
ages are generally only a few Gyr.
- Correction
- Source
- Cite
- Save
- Machine Reading By IdeaReader
71
References
1
Citations
NaN
KQI