On the Differential Rotation of Massive Main Sequence Stars

TL;DR

This paper demonstrates through 2D simulations that internal gravity waves can explain the diverse differential rotation profiles observed in massive main-sequence stars, predicting specific rotation behaviors in high-mass, fast rotators.

Contribution

It introduces a 2D simulation model showing that internal gravity waves account for observed stellar rotation profiles, advancing understanding of angular momentum transport.

Findings

IGW can explain observed rotation profiles

Predicted positive core-envelope differential rotation in high-mass stars

Simulation results align with asteroseismic measurements

Abstract

To date, asteroseismology has provided core to surface differential rotation measurements in eight main-sequence stars. These stars, ranging in mass from $\sim$1.5-9$M_\odot$, show rotation profiles ranging from uniform to counter-rotation. Although they have a variety of masses, these stars all have convective cores and overlying radiative regions, conducive to angular momentum transport by internal gravity waves (IGW). Using two-dimensional (2D) numerical simulations we show that angular momentum transport by IGW can explain all of these rotation profiles. We further predict that should high mass, faster rotating stars be observed, the core to envelope differential rotation will be positive, but less than one.