On using dipolar modes to constrain the helium glitch in red-giant stars

TL;DR

This study explores how using pure acoustic dipolar mode frequencies can improve the detection and characterization of helium glitches in red-giant stars, providing more accurate seismic constraints on stellar core structures.

Contribution

It demonstrates a method to derive pure dipolar mode frequencies from mixed modes, enhancing the seismic analysis of helium glitches in red giants.

Findings

Pure dipolar mode second differences follow the same oscillatory pattern as radial modes.

Using dipolar modes reduces bias in glitch location estimation.

Glitch amplitude is 15% smaller when using dipolar modes.

Abstract

The space-borne missions CoRoT and Kepler have revealed numerous mixed modes in red-giant stars. These modes carry a wealth of information about red-giant cores, but are of limited use when constraining rapid structural variations in their envelopes. This limitation can be circumvented if we have access to the frequencies of the pure acoustic dipolar modes in red giants, i.e. the dipole modes that would exist in the absence of coupling between gravity and acoustic waves. We present a pilot study aimed at evaluating the implications of using these pure acoustic mode frequencies in seismic studies of the helium structural variation in red giants. The study is based on artificial seismic data for a red-giant-branch stellar model, bracketing seven acoustic dipole radial orders around vmax. The pure acoustic dipole-mode frequencies are derived from a fit to the mixed-mode period spacings and then used to compute the pure acoustic dipole-mode second differences. The pure acoustic dipole-mode second differences inferred through this procedure follow the same oscillatory function as the radial modes second differences. The additional constraints brought by the dipolar modes allow us to adopt a more complete description of the glitch signature when performing the fit to the second differences. The amplitude of the glitch retrieved from this fit is 15% smaller than that from the fit based on the radial modes alone. Also, we find that thanks to the additional constraints, a bias in the inferred glitch location, found when adopting the simpler description of the glitch, is avoided.