Convection and convective overshooting in stars more massive than 10 M_\odot

2015/05/12 by Jie Jin, Jie, Jin, Chunhua Zhu +3
Physics and Astronomy · #Astronomy and Astrophysical Research #FOS: Physical sciences #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies

paper · pdf · doi:10.48550/arxiv.1505.03182

openalex publication_date 2015/05/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28

Abstract

In this paper, four sets of evolutionary models are computed with different values of the mixing length parameter α_{\rm p} and the overshooting parameter δ_{\rm ov}. The properties of the convective cores and the convective envelopes are studied in the massive stars. We get three conclusions: First, the larger α_{\rm p} leads to enhancing the convective mixing, removing the chemical gradient, and increasing the convective heat transfer efficiency. Second, core potential ϕ_{\rm c} = M_{\rm c} / R_{\rm c} describes sufficiently the evolution of a star, whether it is a red or blue supergiant at central helium ignition. Third, the discontinuity of hydrogen profile above the hydrogen burning shell seriously affect the occurrence of blue loops in the Hertzsprung--Russell diagram.

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