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

Key physical ingredients governing the evolution of massive stars are masslosses, convection and mixing in radiative zones. These effects are importantboth in the frame of single and close binary evolution. The present paperaddresses two points: 1) the differences between two families of rotatingmodels, i.e. the family of models computed with and without an efficienttransport of angular momentum in radiative zones; 2) The impact of the masslosses in single and in close binary models.

Physics of massive stars relevant for the modeling of Wolf-Rayet populations