Gravitational Radiation from the radial infall of highly relativistic point particles into Kerr black holes

Details Gravitational Radiation from the radial infall of highly relativistic point particles into Kerr black holes Gravitational Radiation from the radial infall of highly relativistic point particles into Kerr black holes

2002-11-27

arxiv.org/abs/gr-qc/0211094v2

Phys.Rev.D67:084005,2003

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

15 pages, REVTEX4. Some comments and references added

Scientific paper

10.1103/PhysRevD.67.084005

In this paper, we consider the gravitational radiation generated by the collision of highly relativistic particles with rotating Kerr black holes. We use the Sasaki-Nakamura formalism to compute the waveform, energy spectra and total energy radiated during this process. We show that the gravitational spectrum for high-energy collisions has definite characteristic universal features, which are independent of the spin of the colliding objects. We also discuss possible connections between these results and the black hole-black hole collision at the speed of light process. With these results at hand, we predict that during the high speed collision of a non-rotating hole with a rotating one, about 35% of the total energy can get converted into gravitational waves. Thus, if one is able to produce black holes at the Large Hadron Collider, as much as 35% of the partons' energy should be emitted during the so called balding phase. This energy will be missing, since we don't have gravitational wave detectors able to measure such amplitudes. The collision at the speed of light between one rotating black hole and a non-rotating one or two rotating black holes turns out to be the most efficient gravitational wave generator in the Universe.

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