  We investigate non-radial oscillations of pure and hybrid neutron stars,
employing equations of state of nuclear matter from Brueckner-Hartree-Fock
theory, and of quark matter from the Dyson-Schwinger quark model, performing a
Gibbs construction for the mixed phase in hybrid stars. Characteristic
differences between neutron-star and hybrid-star $g_1$-mode oscillation
frequencies, damping times, and gravitational wave strains are pointed out.
Prospects of observations are also discussed.
