  We describe the dynamical behavior of newborn pulsars modeled as homogeneous
rotating spheroids. The dynamical evolution is triggered by the escape of
trapped neutrinos, provided the initial equilibrium configuration. It is shown
that for a given set of values of the initial angular momentum a shape
transition to a triaxial ellipsoid configuration occurs. Gravitational waves
are then generated by the breaking of the axial symmetry, and some aspects of
their observation are discussed. We found a narrow window for the initial
values of the angular frequency and the eccentricity able to enable a dynamical
shape transition, with the Kepler frequency of the rotating fluid determining
the upper bound of the initial angular frequency and eccentricity. The loss of
energy and angular momentum carried away by the gravitational wave is treated
consistently with the solution of the equations of motion, which govern the
dynamical evolution of the system. The transition in the shape of the core of
the pulsar is weakly dependent on the time scale of the neutrino escape.
