Models of $\mu$ Her with asteroseismic constraints

TL;DR

This study models mu Her using asteroseismic data and stellar evolution codes, constraining its properties and evolutionary stage with high precision, and highlights the importance of asteroseismology in stellar modeling.

Contribution

It presents the first detailed asteroseismic modeling of mu Her, refining its fundamental parameters and demonstrating the utility of asteroseismic constraints in stellar evolution models.

Findings

Estimated mass of 1.00^{+0.01}_{-0.02} M_sun

Age determined as 6.433 ± 0.04 Gyr

Models with 1.00 - 1.10 M_sun fit observations

Abstract

Using the Yale stellar evolution code, models of mu Her based on asteroseismic measurements are constructed. A $\chi^{2}$ minimization is performed to approach the best modeling parameters which reproduce the observations within their errors. By combining all non-asteroseismic constraints with asteroseismic measurements, we find that the observational constraints favour a model with a mass of 1.00$^{+ 0.01}_{- 0.02}$ $M_{\odot}$, an age t = 6.433 $\pm$ 0.04 Gyr, a mixing-length parameter $\alpha$ = 1.75 $\pm$ 0.25, an initial hydrogen abundance $X_{i}$ = 0.605$^{+ 0.01}_{- 0.005}$ and metal abundance $Z_{i}$ = 0.0275$^{+ 0.002}_{- 0.001}$. mu Her is in post-main sequence phase of evolution. The modes of $l$ = 1 show up the characteristics of avoided crossings, which may be applied to test the internal structure of this type stars. Asteroseismic measurements can be used as a complementary constraint on the modeling parameters. The models with mass 1.00 - 1.10 $M_{\odot}$ can reproduce the observational constraints. Existing observed data of mu Her do not rule out these models.