  Several classes of stars (most notably O and B main-sequence stars, as well
as accreting white dwarfs and neutron stars) rotate quite rapidly, at spin
frequencies greater than the typical g-mode frequencies. We discuss how rapid
rotation modifies the $\kappa$-mechanism excitation and observability of g-mode
oscillations. We find that, by affecting the timescale match between the mode
period and the thermal time at the driving zone, rapid rotation stabilizes some
of the g-modes that are excited in a non-rotating star, and, conversely,
excites g-modes that are damped in absence of rotation. The fluid velocities
and temperature perturbations are strongly concentrated near the equator for
most g-modes in rapidly rotating stars, which means that a favorable viewing
angle may be required to observe the pulsations. Moreover, the stability of
modes of the same $l$ but different $m$ is affected differently by rotation. We
illustrate this by considering g-modes in Slowly Pulsating B-type stars as a
function of the rotation rate.
