  The frequencies and damping times of the non radial oscillations of neutron
stars are computed for a set of recently proposed equations of state (EOS)
which describe matter at supranuclear densites. These EOS are obtained within
two different approaches, the nonrelativistic nuclear many-body theory and the
relativistic mean field theory, that model hadronic interactions in different
ways leading to different composition and dynamics. Being the non radial
oscillations associated to the emission of gravitational waves, we fit the
eigenfrequencies of the fundamental mode and of the first pressure and
gravitational-wave mode (polar and axial) with appropriate functions of the
mass and radius of the star, comparing the fits, when available, with those
obtained by Andersson and Kokkotas in 1998. We show that the identification in
the spectrum of a detected gravitational signal of a sharp pulse corresponding
to the excitation of the fundamental mode or of the first p-mode, combined with
the knowledge of the mass of the star - the only observable on which we may
have reliable information - would allow to gain interesting information on the
composition of the inner core. We further discuss the detectability of these
signals by gravitational detectors.
