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Recent observations of Rossby waves and other more exotic forms of inertialoscillations in the Sun's convection zone have kindled the hope that such wavesmight be used as a seismic probe of the Sun's interior. Here we present a 3Dnumerical simulation in spherical geometry that models the Sun's convectionzone and upper radiative interior. This model features a wide variety ofinertial oscillations, including both sectoral and tesseral equatorial Rossbywaves, retrograde mixed inertial modes, prograde thermal Rossby waves, therecently observed high-frequency retrograde (HFR) vorticity modes, and what maybe latitudinal overtones of these HFR modes. With this model, we demonstratethat sectoral and tesseral Rossby waves are ubiquitous within the radiativeinterior as well as within the convection zone. We suggest that there are twodifferent Rossby-wave families in this simulation that live in different wavecavities: one in the radiative interior and one in the convection zone.Finally, we suggest that many of the retrograde inertial waves that appear inthe convection zone, including the HFR modes, are in fact all related, beinglatitudinal overtones that are mixed modes with the prograde thermal Rossbywaves.

Inertial Waves in a Nonlinear Simulation of the Sun's Convection Zone and Radiative Interior