Effect of Rotation on Wave Mixing in Intermediate Mass Stars

TL;DR

This study investigates how stellar rotation affects internal gravity wave-induced mixing in intermediate mass stars, revealing that increased rotation suppresses mixing due to altered convection dynamics.

Contribution

It provides new insights into the impact of rotation rates on wave mixing profiles in 7 solar mass stars at different evolutionary stages.

Findings

Mixing decreases with increasing rotation rate.

Rotation influences wave excitation amplitude near the convective-radiative interface.

The effect is linked to changes in convection caused by rotation.

Abstract

Internal gravity waves (IGWs) are likely to cause mixing in stellar interiors. Studies show that the mixing by these waves changes drastically across age and mass (Varghese et al. 2023, arXiv:2211.06432). Here, we study the effect of rotation on this wave mixing by considering a 7 M$_{\odot}$ model at ZAMS and midMS. We compare the mixing profiles at a range of rotation rates ($1\times 10^{-5}$, $2\times 10^{-5}$, $3\times 10^{-5}$, $4\times 10^{-5}$ and $1\times 10^{-4}$ rad.s$^{-1}$) and observe that the mixing decreases with decreasing Rossby number. This can be attributed to the effect of rotation on convection which influences the amplitude with which the waves are excited near the convective-radiative interface.