2024ApJ...974...77L

Asteroseismic modeling is a powerful way to derive stellar properties. However, the derived quantities are limited by built-in assumptions used in stellar models. This work presents a detailed characterization of stellar model uncertainties in asteroseismic red giants, focusing on the mixing-length parameter α_MLT, the initial helium fraction Y_init, the solar abundance scale, and the overshoot parameters. First, we estimate error floors due to model uncertainties to be ≈0.4% in mass, ≈0.2% in radius, and ≈17% in age, primarily due to the uncertain state of α_MLT and Y_init. The systematic uncertainties in age exceed typical statistical uncertainties, suggesting the importance of their evaluation in asteroseismic applications. Second, we demonstrate that the uncertainties from α_MLT can be entirely mitigated by direct radius measurements or partially through ${\nu }_{\max }$. Utilizing radii from Kepler eclipsing binaries, we determined the α_MLT values and calibrated the α_MLT-[M/H] relation. The correlation observed between the two variables is positive, consistent with previous studies using 1D stellar models, but in contrast with outcomes from 3D simulations. Third, we explore the implications of using asteroseismic modeling to test the ${\nu }_{\max }$ scaling relation. We found that a perceived dependency of ${\nu }_{\max }$ on [M/H] from individual frequency modeling can be largely removed by incorporating the calibrated α_MLT-[M/H] relation. Variations in Y_init can also affect ${\nu }_{\max }$ predictions. These findings suggest that ${\nu }_{\max }$ conveys information not fully captured by individual frequencies, and that it should be carefully considered as an important observable for asteroseismic modeling.