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arXiv · 1807.08766

Enhanced Rotational Mixing in the Radiative Zones of Massive Stars

Adam S. Jermyn·Christopher A. Tout·Shashikumar M. Chitre
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Abstract

Convection in the cores of massive stars becomes anisotropic when they rotate. This anisotropy leads to a misalignment of the thermal gradient and the thermal flux, which in turn results in baroclinicity and circulation currents in the upper radiative zone. We show that this induces a much stronger meridional flow in the radiative zone than previously thought. This drives significantly enhanced mixing, though this mixing does not necessarily reach the surface. The extra mixing takes on a similar form to convective overshooting, and is relatively insensitive to the rotation rate above a threshold, and may help explain the large overshoot distances inferred from observations. This has significant consequences for the evolution of these stars by enhancing core-envelope mixing.

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Adam S. Jermyn, Christopher A. Tout, Shashikumar M. Chitre. 2018-10-24. Enhanced Rotational Mixing in the Radiative Zones of Massive Stars. https://doi.org/10.1093/mnras%2Fsty1831

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