The effects of rotation on wave-induced transport in stars: from weakly to strongly stratified radiative zones. (arXiv:1811.02818v1 [astro-ph.SR])

The effects of rotation on wave-induced transport in stars: from weakly to strongly stratified radiative zones. (arXiv:1811.02818v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Andre_Q/0/1/0/all/0/1">Q. Andr&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mathis_S/0/1/0/all/0/1">S. Mathis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amard_L/0/1/0/all/0/1">L. Amard</a>

Internal waves propagating in stellar radiative zones can lead to efficient
angular momentum transport, that should occur throughout the whole lifetime of
stars. They thus play a key role in shaping the internal rotation profile of
these regions, that can be probed by asteroseismology. We present a new
analytical study of their propagation and dissipation near the equatorial
plane. We include the effects of rotation and differential rotation without
making any assumption on their relative strength relative to that of the
background stable stratification. This analytical framework allows in principle
to scan the efficiency of the wave-induced transport of angular momentum. The
computations goes from the pre-main sequence, during which the restoring forces
associated with rotation and stratification can be of the same order, to the
later stages of evolution, for which stratification tends to dominate over
rotation. A first application to the case of a sun-like star is finally
discussed.

Internal waves propagating in stellar radiative zones can lead to efficient
angular momentum transport, that should occur throughout the whole lifetime of
stars. They thus play a key role in shaping the internal rotation profile of
these regions, that can be probed by asteroseismology. We present a new
analytical study of their propagation and dissipation near the equatorial
plane. We include the effects of rotation and differential rotation without
making any assumption on their relative strength relative to that of the
background stable stratification. This analytical framework allows in principle
to scan the efficiency of the wave-induced transport of angular momentum. The
computations goes from the pre-main sequence, during which the restoring forces
associated with rotation and stratification can be of the same order, to the
later stages of evolution, for which stratification tends to dominate over
rotation. A first application to the case of a sun-like star is finally
discussed.

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