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Gravito-inertial waves are excited at the interface of convective andradiative regions and by the Reynolds stresses in the bulk of the convectionzones of rotating stars and planets. Such waves have notable asteroseismicsignatures in the frequency spectra of rotating stars, particularly amongrapidly rotating early-type stars, which provides a means of probing theirinternal structure and dynamics. They can also transport angular momentum,chemical species, and energy from the excitation region to where they dissipatein radiative regions. To estimate the excitation and convective parameterdependence of the amplitude of those waves, a monomodal model for stellar andplanetary convection as described in Paper I is employed, which provides themagnitude of the rms convective velocity as a function of rotation rate. Withthis convection model, two channels for wave driving are considered: excitationat a boundary between convectively stable and unstable regions and excitationdue to Reynolds-stresses. Parameter regimes are found where the sub-inertialwaves may carry a significant energy flux, depending upon the convective Rossbynumber, the interface stiffness, and the wave frequency. The super-inertialwaves can also be enhanced, but only for convective Rossby numbers near unity.Interfacially excited waves have a peak energy flux near the lower cutofffrequency when the convective Rossby number of the flows that excite them arebelow a critical Rossby number that depends upon the stiffness of theinterface, whereas that flux decreases when the convective Rossby number islarger than this critical Rossby number.

A model of rotating convection in stellar and planetary interiors: II -- gravito-inertial wave generation