MG11 
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Gravitational waves from three-dimensional simulations of rotating neutron-star collapse

We present our results on the computation of the gravitational-wave radiation emitted during the collapse of a uniformly rotating neutron star to a Kerr black hole. In our three-dimensionsal simulations, no excision is performed once an apparent horizon is found. We show that this choice, combined with suitable gauge conditions and the use of numerical dissipation inside and outside the apparent horizon, improves dramatically the long-term stability of the evolutions. In turn, this allows for the calculation of the gravitational waveforms well beyond what previously possible, providing information on the black hole quasi-normal ringing and considerably improving the present knowledge of the gravitational-wave emission from a rotating collapse to a black hole.