  We investigate the impact of charged current neutrino processes on the
formation and evolution of neutrino spectra during the deleptonization of
proto-neutron stars. To this end we develop the full kinematics of these
reaction rates consistent with the nuclear equation of state, including weak
magnetism contributions. This allows us to systematically study the impact of
inelastic contributions and weak magnetism on the $\nu_e$ and $\bar\nu_e$
luminosities and average energies. Furthermore, we explore the role of the
inverse neutron decay, also known as the direct Urca process, on the emitted
spectra of $\bar\nu_e$. This process is commonly considered in the cooling
scenario of cold neutron stars but has so far been neglected in the evolution
of hot proto-neutron stars. We find that the inverse neutron decay becomes the
dominating opacity source for low-energy $\bar\nu_e$. Accurate three-flavor
Boltzmann neutrino transport enables us to relate the magnitude of neutrino
fluxes and spectra to details of the treatment of weak processes. This allows
us to quantify the corresponding impact on the conditions relevant for the
nucleosynthesis in the neutrino-driven wind, which is ejected from the
proto-neutron star surface during the deleptonization phase.
