Mixed Mode Asteroseismology of Red Giant Stars Through the Luminosity Bump

Abstract

Most current models of low mass red giant stars do not reproduce the observed position of the red giant branch luminosity bump, a diagnostic of the maximum extent of the convective envelope during the first dredge up. Global asteroseismic parameters, the large frequency separation and frequency of maximum oscillation power, measured for large samples of red giants, show that modeling convective overshoot below the convective envelope helps match the modeled luminosity bump positions to observations. However, these global parameters cannot be used to probe envelope overshoot in a star-by-star manner. Red giant mixed modes, which behave like acoustic modes at the surface and like gravity modes in the core, contain important information about the interior structure of the star, especially near the convective boundary. Therefore, these modes may be used to probe interior processes, such as overshoot. Using a grid of red giant models with varying mass, metallicity, surface gravity, overshoot treatment, and amount of envelope overshoot, we find that changing the overshoot amplitude (and prescription) of overshoot below the convection zone in red giant stellar models results in significant differences in the evolution of the models' dipole mixed-mode oscillation frequencies, the average mixed mode period spacing, $⟨\Delta P⟩$, and gravity mode phase offset term, ${\epsilon }_g$.

19 pages, 16 figures. Accepted for publication in ApJ April 18 2022

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• Asteroseismic measurement of core and envelope rotation rates for 2006 red giant branch stars
• Mode Mixing and Rotational Splittings: II. Reconciling Different Approaches to Mode Coupling
• Near-Core Acoustic Glitches are Not Oscillatory: Consequences for Asteroseismic Probes of Convective Boundary Mixing
• Acoustic modes in M67 cluster stars trace deepening convective envelopes
• TESS Asteroseismic Analysis of HD 76920: The Giant Star Hosting An Extremely Eccentric Exoplanet
• Pushing the boundaries of asteroseismic individual frequency modelling: unveiling two evolved very-low metallicity red giants
• Inferring the efficiency of convective-envelope overshooting in Red Giant Branch stars
• Realising efficient computation of individual frequencies for red-giant models