Convection and convective overshooting in stars more massive than 10 $M_\odot$
Abstract
In this paper, four sets of evolutionary models are computed with different values of the mixing length parameter $\alpha_{\rm p}$ and the overshooting parameter $\delta_{\rm ov}$. The properties of the convective cores and the convective envelopes are studied in the massive stars. We get three conclusions: First, the larger $\alpha_{\rm p}$ leads to enhancing the convective mixing, removing the chemical gradient, and increasing the convective heat transfer efficiency. Second, core potential $\phi_{\rm c} = M_{\rm c} / R_{\rm c}$ 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.
- Publication:
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arXiv e-prints
- Pub Date:
- May 2015
- DOI:
- 10.48550/arXiv.1505.03182
- arXiv:
- arXiv:1505.03182
- Bibcode:
- 2015arXiv150503182J
- Keywords:
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- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- 6 pages, 5 figures, accepted for publication by PASJ