Equatorial Kelvin waves in a differentially rotating spherical shell can be destabilized by suitable levels of radial differential rotation and viscosity, potentially contributing to the Be-star excretion mechanism.
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Kelvin waves over a differentially rotating spherical shell
Equatorial Kelvin waves in a differentially rotating spherical shell can be destabilized by suitable levels of radial differential rotation and viscosity, potentially contributing to the Be-star excretion mechanism.