Gravitational Radiation from 3D Collapse to Rotating Black Holes

Details Gravitational Radiation from 3D Collapse to Rotating Black Holes Gravitational Radiation from 3D Collapse to Rotating Black Holes

Feb 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006nwap.conf..147b&link_type=abstract

NEW WORLDS IN ASTROPARTICLE PHYSICS. Proceedings of the Fifth International Workshop. Held 8-10 January 2005 in Faro, Portugal.

Physics

Scientific paper

We discuss the application of our new three-dimensional fully general relativistic hydrodynamics code which uses high-resolution shock-capturing techniques and a conformal traceless formulation of the Einstein equations, to the study of the gravitational collapse of uniformly rotating neutron stars to Kerr black holes. We investigate the dynamics of the matter and of the trapped surfaces and provide precise measurements of the black-hole mass and spin. We also present the first calculation of the gravitational wave emission produced in fully three-dimensional simulations. An essential aspect of these simulations is the use of progressive mesh-refinement techniques which allow to move the outer boundaries of the computational domain to regions where gravitational radiation attains its asymptotic form. The waveforms have been extracted using a gauge-invariant approach in which the numerical spacetime is matched with the non-spherical perturbations of a Schwarzschild spacetime. Overall, the results indicate that the waveforms have features related to the properties of the initial stellar models (in terms of their w-mode oscillations) and of the newly produced rotating black holes (in terms of their quasi-normal modes). While our waveforms are in good qualitative agreement with those computed in two-dimensional simulations, our amplitudes are about one order of magnitude smaller and this difference is most likely due to our less severe pressure reduction. For a neutron star rotating uniformly near mass-shedding and collapsing at 10 kpc, the signal-to-noise ratio computed uniquely from the burst is S/N ˜ 0.25 for LIGO/VIRGO, but this grows to be S/N ≲ 4 for LIGO II.

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