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

Double-line eclipsing binaries (DLEBs) have been recently used to constrainthe amount of central mixing as a function of stellar mass, with contrastingresults. In this work, we reanalyze the DLEB sample by Claret & Torres, using aBayesian method and new PARSEC tracks that account for both convective coreovershooting and rotational mixing. Using overshooting alone we obtain that,for masses larger than about 1.9 M$_{\odot}$, the distribution of theovershooting parameter, $\lambda_\mathrm{ov}$, has a wide dispersion between0.3 and 0.8, with essentially no values below $\lambda_\mathrm{ov}=$ 0.3 - 0.4.While the lower limit supports a mild convective overshooting efficiency, thelarge dispersion derived is difficult to explain in the framework of currentmodels of that process, which leave little room for large randomness. Wesuggest that a simple interpretation of our results can be rotational mixing:different initial rotational velocities, in addition to a fixed amount ofovershooting, could reproduce the high dispersion derived for intermediate-massstars. After a reanalysis of the data, we find good agreement with modelscomputed with fixed overshooting parameter, $\lambda_\mathrm{ov}=0.4$, andinitial rotational rates, $\omega$, uniformly distributed in a wide rangebetween $0$ and $0.8$ times the break-up value, at varying initial mass. Wealso find that our best-fitting models for the components of $\alpha$ Aurigaeand TZ Fornacis, agree with their observed rotational velocities, thusproviding independent support to our hypothesis. We conclude that a constantefficiency of overshooting in concurrence with a star-to-star variation in therotational mixing, might be crucial in the interpretation of such data.

Mixing by overshooting and rotation in intermediate mass stars