  The $\kappa$-mechanism has been successful in explaining the origin of
observed oscillations of many types of "classical" pulsating variable stars.
Here we examine quantitatively if that same process is prominent enough to
excite the potential global oscillations within Jupiter, whose energy flux is
powered by gravitational collapse rather than nuclear fusion. Additionally, we
examine whether external radiative forcing, i.e. starlight, could be a driver
for global oscillations in hot Jupiters orbiting various main-sequence stars at
defined orbital semimajor axes. Using planetary models generated by the Modules
for Experiments in Stellar Astrophysics (MESA) and nonadiabatic oscillation
calculations, we confirm that Jovian oscillations cannot be driven via the
$\kappa$-mechanism. However, we do show that in hot Jupiters oscillations can
likely be excited via the suppression of radiative cooling due to external
radiation given a large enough stellar flux and the absence of a significant
oscillatory damping zone within the planet. This trend seems to not be
dependent on the planetary mass. In future observations we can thus expect that
such planets may be pulsating, thereby giving greater insight into the internal
structure of these bodies.
