The effects of near-core convective shells on the gravity modes of the subdwarf B pulsator KIC 10553698A

TL;DR

This study investigates how near-core convective shells caused by different levels of overshooting affect the gravity mode patterns in a pulsating subdwarf B star, using stellar models aligned with Kepler observations.

Contribution

It demonstrates that convective shells significantly influence g-mode period spacings and provides models with overshooting and diffusion that match observed seismic data.

Findings

Convective shells alter g-mode period spacing patterns.

Moderate and small overshooting models match observed period spacings.

Atomic diffusion improves model-observation agreement.

Abstract

KIC 10553698A is a hot pulsating subdwarf B (sdB) star observed by the Kepler satellite. It exhibits dipole (l = 1) and quadrupole (l = 2) gravity modes with a clear period spacing structure. The seismic properties of the KIC 10553698A provide a test of stellar evolution models, and offer a unique opportunity to determine mixing processes. We consider mixing due to convective overshooting beyond the boundary of the helium burning core. Very small overshooting ( f = 10^{-6} ) results in a progressive increase in the size of convective core. However, moderate ( f = 10^{-2} ) and small ( f = 10^{-5} ) overshooting both lead to the occurrence of inert outer convective shells in the near-core region. We illustrate that the chemical stratifications induced by convective shells are able to change the g-mode period spacing pattern of a sdB star appreciably. The mean period spacing and trapping of the gravity modes in the model with moderate and small core overshooting are fully consistent with the period spacing trends observed in KIC 10553698A. Atomic diffusion driven by gravitational settling as well as thermal and chemical gradients is applied to reach a better match with the observed period spacings. Models that include small or very small overshooting with atomic diffusion have a decreased lifetime of the extreme horizontal branch phase and produce chemical stratification induced by convective shells during helium burning phase. In addition of being consistent with asteroseismology, their calculated values of the R2 parameter are more compatible with the observed R2 values.