Glitch analysis and asteroseismic modelling of subgiant $μ$ Herculis: confirming and interpreting the $Γ_1$ peak as the helium glitch

Le résumé fourni par la source

The measurements of pressure-mode and mixed-mode oscillation frequencies in subgiant stars offer a unique opportunity to probe their internal structures -- from the surface to the deep interior -- and to precisely determine their global properties. We have conducted a detailed asteroseismic analysis of the benchmark subgiant $μ$ Herculis using eight seasons of radial velocity observations from the SONG-Tenerife, and have determined its mass, radius, age, and surface helium abundance to be $1.105_{-0.024}^{+0.058}$ M$_\odot$, $1.709_{-0.015}^{+0.030}$ R$_\odot$, $8.4_{-0.1}^{+0.4}$ Gyr, and $0.242^{+0.006}_{-0.021}$, respectively. We have demonstrated that simultaneously fitting the helium glitch properties, oscillation frequencies, and spectroscopic observables yields a more accurate inference of the surface helium abundance and hence stellar age. A significant discrepancy between the observed extent of the helium ionization zone and that predicted by stellar models is identified and examined, underscoring potential limitations in the current modelling of stellar interiors. Our analysis confirms that the helium glitch originates from the region between the two stages of helium ionisation, i.e. from the $Γ_1$ peak, rather than from the second helium ionisation zone itself. Within the conventional formalism, this implies that the glitch analysis characterises the region located between the two helium ionisation zones.

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