Detailed calculations are made of the neutrino spectra emitted during gravitational collapse events (Type II supernovae? ). Those aspects of the neut.rino signal which are relatively independent of the collapse model and those aspects which are sensitive to model details are discussed. The easier-to-detect high energy tail of the emitted neutrinos has been calculated using the Eloltzmann equation which is compared with t,he result of the traditional multi-group flux limited diffusion calculations.