Gravito-inertial modes in a differentially rotating spherical shell
1 Université de Toulouse, UPS-OMP, IRAP, Toulouse, France
2 CNRS, IRAP, 14 avenue Edouard Belin, 31400 Toulouse, France
a e-mail: firstname.lastname@example.org
Published online: 23 September 2015
While many intermediate- and high-mass main sequence stars are rapidly and differentially rotating, the effects of rotation on oscillation modes are poorly known. In this communication we present a first study of axisymmetric gravito-inertial modes in the radiative zone of a differentially rotating star. We consider a simplified model where the radiative zone of the star is a linearly stratified rotating fluid within a spherical shell, with differential rotation due to baroclinic effects. We solve the eigenvalue problem with high-resolution spectral computations and determine the propagation domain of the waves through the theory of characteristics. We explore the propagation properties of two kinds of modes: those that can propagate in the entire shell and those that are restricted to a sub-domain. Some of the modes that we find concentrate kinetic energy around short-period shear layers known as attractors. We describe various geometries for the propagation domains, conditioning the surface visibility of the corresponding modes.
© Owned by the authors, published by EDP Sciences, 2015
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