Astrophysical rotating fluids
You may face rotating fluids in astrophysics when you are considering
stars in binary systems: tidal effect usually locks the spin rotation of
the stars to that of their orbital motion; when periods are short (typically
less than a few days) the Coriolis force is controlling most of the flows
inside the stars and the fluid is said to be rotating. More about that
may be found in:
But stars may rotate alone because they are young and still have a lot
of angular momentum of the cloud which gave them birth. Their period may
be around one day which is very fast (the surface velocity is often not
much less than the keplerian velocity). Sometimes they oscillate (they
are then called Gamma Dor, Delta Scuti, Dzeta Oph etc...) and we wish to
model these oscillations because they allow us to understand their
internal structure; now start the difficulties because such oscillations
are much perturbed by the Coriolis force; you will now read:
Rieutord M. and Bonazzola S. (1987),"Tidal heating in close binary stellar
systems" Monthly Notices of the Royal Astronomical Society, vol. 227, pp.~295--314.
Rieutord M. (1992), "Ekman circulation and the synchronization of binary
stars". Astronomy and Astrophysics, vol. 259, pp.~581--584.
Rieutord M. and Zahn J.-P. (1997), "Ekman pumping and tidal dissipation
in close binary stars: a refutation of Tassoul's mechanism", Astrophys.
J. vol. 474, pp.~760--767.
Dintrans B. and Rieutord M. (2000),"Oscillations of a rotating star: a
non-perturbative theory", Astron. Astrophys., vol. 354, p. 86-98,