  We study how the frequencies and damping times of oscillations of a newly
born, hot proto-neutron star depend on the physical quantities which
characterize the star quasi-stationary evolution which follows the bounce.
Stellar configurations are modeled using a microscopic equation of state
obtained within the Brueckner-Hartree-Fock, nuclear many-body approach,
extended to the finite-temperature regime. We discuss the mode frequency
behaviour as function of the lepton composition, and of the entropy gradients
which prevail in the interior of the star. We find that, in the very early
stages, gravitational wave emission efficiently competes with neutrino
processes in dissipating the star mechanical energy residual of the
gravitational collapse.
