  We present the results of a numerical study of the fluid $f$, $p$ and the
gravitational $w$ modes for increasingly relativistic nonrotating polytropes.
The results for $f$ and $w$-modes are in good agreement with previous data for
uniform density stars, which supports an understanding of the nature of the
gravitational wave modes based on the uniform density data. We show that the
$p$-modes can become extremely long-lived for some relativistic stars. This
effect is attributed to the change in the perturbed density distribution as the
star becomes more compact.
