Generation of Post-Newtonian Gravitational Radiation via Direct Integration of the Relaxed Einstein Equations

Details Generation of Post-Newtonian Gravitational Radiation via Direct Integration of the Relaxed Einstein Equations Generation of Post-Newtonian Gravitational Radiation via Direct Integration of the Relaxed Einstein Equations

1999-10-15

arxiv.org/abs/gr-qc/9910057v1

Prog.Theor.Phys.Suppl.136:158-167,1999

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

11 pages, PTPTeX, submitted to Proceedings of the Yukawa-Kyoto International Seminar 99

Scientific paper

10.1143/PTPS.136.158

The completion of a network of advanced laser-interferometric gravitational-wave observatories around 2001 will make possible the study of the inspiral and coalescence of binary systems of compact objects (neutron stars and black holes), using gravitational radiation. To extract useful information from the waves, such as the masses and spins of the bodies, theoretical general relativistic gravitational waveform templates of extremely high accuracy will be needed for filtering the data, probably as accurate as $O[(v/c)^6]$ beyond the predictions of the quadrupole formula. We summarize a method, called DIRE, for Direct Integration of the Relaxed Einstein Equations, which extends and improves an earlier framework due to Epstein and Wagoner, in which Einstein's equations are recast as a flat spacetime wave equation with source composed of matter confined to compact regions and gravitational non-linearities extending to infinity. The new method is free of divergences or undefined integrals, correctly predicts all gravitational wave ``tail'' effects caused by backscatter of the outgoing radiation off the background curved spacetime, and yields radiation that propagates asymptotically along true null cones of the curved spacetime. The method also yields equations of motion through $O[(v/c)^4]$, radiation-reaction terms at $O[(v/c)^5]$ and $O[(v/c)^7]$, and gravitational waveforms and energy flux through $O[(v/c)^4]$, in agreement with other approaches. We report on progress in evaluating the $O[(v/c)^6]$ contributions.

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