Gravitational radiation during fragmentation of a rotating neutron star

We present calculations of the evolution of a rotating neutron star that is unstable to the development of a sectorial mode which causes fragmentation . The equation of state was chosen to be that of a cold degenerate neutron gas, P proportional to rho(5/3). The mass and angular momentum of the star were taken to be the same as those for a collapsing, rigidly rotating, iron -oxygen stellar core: M = 2M(.) and J = 8 x 10(49) erg s, respectively. The choice of the rotation law for which the ratio of the centrifugal force to the gravity is constant completes the construction of the initial model. A s a result of its evolution, the star loses part of its mass and angular mo mentum and decreases the rotation energy -E-k/E-gr from 0.35 to 0.19. The g ravitational radiation calculated in the quadrupole approximation carries a way the energy 8.4 x 10(49) erg and the angular momentum 1.0 x 10(47) erg s . The typical metric perturbation is rh similar to 10(4) cm, and the wave f requency is similar to 1 kHz.