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      Exact Gravitational Wave Signatures from Colliding Extreme Black Holes

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          Abstract

          The low-energy dynamics of any system admitting a continuum of static configurations is approximated by slow motion in moduli (configuration) space. Here, this moduli space approximation is utilized to study collisions of two maximally charged Reissner-Nordstr\"om black holes of arbitrary masses, and to compute analytically the gravitational radiation generated by their scattering or coalescence. The motion remains slow even though the fields are strong, and the leading radiation is quadrupolar. A simple expression for the gravitational waveform is derived and compared at early and late times to expectations.

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          Evolution of Binary Black Hole Spacetimes

          Frans Pretorius (2005)
          We describe early success in the evolution of binary black hole spacetimes with a numerical code based on a generalization of harmonic coordinates. Indications are that with sufficient resolution this scheme is capable of evolving binary systems for enough time to extract information about the orbit, merger and gravitational waves emitted during the event. As an example we show results from the evolution of a binary composed of two equal mass, non-spinning black holes, through a single plunge-orbit, merger and ring down. The resultant black hole is estimated to be a Kerr black hole with angular momentum parameter a~0.70. At present, lack of resolution far from the binary prevents an accurate estimate of the energy emitted, though a rough calculation suggests on the order of 5% of the initial rest mass of the system is radiated as gravitational waves during the final orbit and ringdown.
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            A Class of Exact Solutions of Einstein's Field Equations

            Sudhansu Majumdar (1947)
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              Effective one-body approach to general relativistic two-body dynamics

              T. Damour, A Buonanno (1998)
              We map the general relativistic two-body problem onto that of a test particle moving in an effective external metric. This effective-one-body approach defines, in a non-perturbative manner, the late dynamical evolution of a coalescing binary system of compact objects. The transition from the adiabatic inspiral, driven by gravitational radiation damping, to an unstable plunge, induced by strong spacetime curvature, is predicted to occur for orbits more tightly bound than the innermost stable circular orbit in a Schwarzschild metric of mass M = m1 + m2. The binding energy, angular momentum and orbital frequency of the innermost stable circular orbit for the time-symmetric two-body problem are determined as a function of the mass ratio.
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                Author and article information

                Journal
                Publication date Created: 2017-04-27
                Article
                ArXiV ID: 1704.08520
                SO-VID: 633fcf5c-8903-4f51-bdf1-c8e905a44b2a
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                http://arxiv.org/licenses/nonexclusive-distrib/1.0/

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                Report No DAMTP-2017-18
                Comments 6 pages
                Categories gr-qc hep-th

                ScienceOpen disciplines: General relativity & Quantum cosmology,High energy & Particle physics
                Data availability:
                ScienceOpen disciplines: General relativity & Quantum cosmology, High energy & Particle physics

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