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We study how the frequencies and damping times of oscillations of a newlyborn, hot proto-neutron star depend on the physical quantities whichcharacterize the star quasi-stationary evolution which follows the bounce.Stellar configurations are modeled using a microscopic equation of stateobtained within the Brueckner-Hartree-Fock, nuclear many-body approach,extended to the finite-temperature regime. We discuss the mode frequencybehaviour as function of the lepton composition, and of the entropy gradientswhich prevail in the interior of the star. We find that, in the very earlystages, gravitational wave emission efficiently competes with neutrinoprocesses in dissipating the star mechanical energy residual of thegravitational collapse.

Oscillations of hot, young neutron stars: Gravitational wave frequencies and damping times