Apsidal Motion in O-Star Binaries: GENEC rotating binary models put to the k2-test

TL;DR

This study uses apsidal motion rates in close eccentric binaries to test and refine stellar models of massive stars, revealing the importance of internal mixing processes and the limitations of current models.

Contribution

The paper introduces bespoke GENEC models with tidal mixing to better match observed stellar density profiles and apsidal motion rates, addressing the k2-discrepancy in massive stars.

Findings

Advecto-diffusive models better reproduce k2 than magnetic models.

Large overshooting is needed to match observed k2.

Higher initial helium abundance improves model agreement.

Abstract

Unveiling massive stars' internal structure and the physical origin and efficiency of the internal mixing processes? It is now possible using the apsidal motion rate in close eccentric binaries! The apsidal motion rate depends on the tidal interactions occurring between the stars and is proportional to k2, a measure of the star's inner density profile. Confronting standard stellar models with observations reveals the famous k2-discrepancy: models predict too high a k2 for the stars, that is to say, stars with too low a density contrast between their core and envelope. We built bespoke GENEC stellar evolution models including tidal mixing for the twin massive binary HD 152248. The models reveal the instabilities allowing to reproduce the stellar density profiles: advecto-diffusive models better reproduce k2 than magnetic models. A large overshooting is necessary to converge towards the observed k2, yet alone is not sufficient. While a change in metallicity or mass-loss rate has no significant impact on k2, a larger initial helium abundance allows us to better reproduce the k2. Yet, a super-solar helium abundance is not observationally supported. Our analyses highlight the need for a process in the stars that slows down the radial expansion.