Post-Newtonian gravitational radiation from binary stars

Details Post-Newtonian gravitational radiation from binary stars Post-Newtonian gravitational radiation from binary stars

Nov 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985gregr..17.1059s&link_type=abstract

General Relativity and Gravitation (ISSN 0001-7701), vol. 17, Nov. 1985, p. 1059-1067.

Physics

5

Binary Stars, Gravitational Waves, Pulsars, Stellar Orbits, Stellar Radiation, Energy Distribution, Quadrupoles, Relativity

Scientific paper

A method based on an energy balance equation, whose results, in view of available observational data, are virtually correct, is used in the present evaluation of post-Newtonian orbital corrections for the orbital period decrease of a relativistic binary. Results previously obtained for the gravitational-radiation luminosity of a bounded source, and of the binary's relative motion, are applied. In the case of the binary pulsar PSR 1913 + 16, the proposed relative orbital correction amounts to about 10 to the -6th of the current observational uncertainty. This result favors the predictions of the classical quadrupole formula.

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