English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The chemical evolution of the Galaxy is largely guided by the yields frommassive stars. Their evolution is heavily influenced by their internal mixing,allowing the stars to live longer and yield a more massive helium core at theend of their main-sequence evolution. Asteroseismology is a powerful tool forstudying stellar interiors by providing direct probes of the interior physicsof the oscillating stars. This work revisits the recently derived internalmixing profiles of 26 slowly pulsating B stars observed by the Kepler spacetelescope, in order to investigate how well the mixing profiles can in fact bedistinguished from one another as well as provide predictions for the expectedhelium core masses obtained at the end of the main-sequence evolution. We findthat for five of these stars the mixing profile is derived unambiguously, whilethe remaining stars have at least one other mixing profile which explains theoscillations equally well. Convective penetration is preferred over exponentialdiffusive overshoot for ~55% of the stars, while stratified mixing is preferredin the envelope (~39%). We estimate the expected helium core masses obtained atthe end of the main-sequence evolution and find them to be highly influenced bythe estimated amount of mixing occurring in the envelopes of the stars.

On the diversity of mixing and helium core masses of B-type dwarfs from gravity-mode asteroseismology