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

Understand

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.