Authors: Catherine Blume (University of Colorado Boulder), Bradley Hindman (University of Colorado Boulder), Loren Matilsky (UC Santa Cruz)

Recent observations of Rossby waves and other more exotic forms of inertial oscillations in the Sun’s convective zone have kindled the hope that such waves might be used as a seismic probe of the Sun’s interior. Here we present a suite of 3D numerical simulations in full spherical geometry that model the Sun’s convective zone and upper radiative interior. With these models, we demonstrate that Rossby waves are ubiquitous within the radiative interior as well as within the convective zone. In characterizing these modes, we find the presence of radial overtones, which complicates our interpretations of Rossby wave observations. We also note that the sectoral modes are the primary waves seen at the surface.