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We reexamine the gravitational collapse of rotating neutron stars to blackholes by new 3+1 numerical relativity simulations employing the Z4c formulationof Einstein equations, the moving puncture gauge conditions, and a conservativemesh refinement scheme for the general relativistic hydrodynamics. The endstate of the collapse is compared to the vacuum spacetime resulting from theevolution of spinning puncture initial data. Using a local analysis for themetric fields, we demonstrate that the two spacetimes actually agree.Gravitational waveforms are analyzed in some detail. We connect the emission ofradiation to the collapse dynamics using simplified spacetime diagrams, anddiscuss the similarity of the waveform structure with the one of black holeperturbation theory.

Simulations of rotating neutron star collapse with the puncture gauge: end state and gravitational waveforms