Properties of the ionisation glitch: I. Modelling the ionisation region

TL;DR

This paper develops an analytical model of the ionisation region in solar-like stars to better understand the ionisation glitch, aiming to improve independent estimates of surface helium abundance and address biases in stellar property determinations.

Contribution

It introduces a thermodynamic approximation for the first adiabatic exponent, enabling a flexible model of the ionisation region that accounts for structural perturbations and dependencies beyond helium content.

Findings

The model depends on three parameters including $Y_s$ and electron degeneracy.

It can approximate realistic stellar models in the ionisation region.

Structural perturbations are more complex than previously assumed.

Abstract

Determining the properties of solar-like oscillating stars can be subject to many biases. A particularly important example is the helium-mass degeneracy, where the uncertainties regarding the internal physics can cause a poor determination of both the mass and surface helium content. Accordingly, an independent helium estimate is needed to overcome this degeneracy. A promising way to obtain such an estimate is to exploit the so-called ionisation glitch, i.e. a deviation from the asymptotic oscillation frequency pattern caused by the rapid structural variation in the He ionisation zones. Although progressively becoming more sophisticated, the glitch-based approach faces problems inherent to its current modelling such as the need for calibration by realistic stellar models. This requires a physical model of the ionisation region explicitly involving the parameters of interest such as the surface helium abundance, $Y_s$. Through a thermodynamic treatment of the ionisation region, an analytical approximation for the first adiabatic exponent $\Gamma_1$ is presented. The induced stellar structure is found to depend on only three parameters including the surface helium abundance $Y_s$ and the electron degeneracy $\psi_\textrm{CZ}$ in the convective region. The model thus defined allows a wide variety of structures to be described and, in particular, is able to approximate a realistic model in the ionisation region. The modelling work conducted enables us to study the structural perturbations causing the glitch. More elaborate forms of perturbations than the ones usually assumed are found. It is also suggested that there might be a stronger dependence of the structure on both the electron degeneracy in the convection zone and on the position of the ionisation region rather than on the amount of helium itself.