The new formula for gravitational-radiation energy loss and the axially symmetric two-body problem

Details The new formula for gravitational-radiation energy loss and the axially symmetric two-body problem The new formula for gravitational-radiation energy loss and the axially symmetric two-body problem

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986cajph..64..134c&link_type=abstract

Canadian Journal of Physics (ISSN 0008-4204), vol. 64, Feb. 1986, p. 134-139. Research supported by the University of Victoria.

Physics

2

Energy Dissipation, Gravitational Waves, Two Body Problem, Binary Stars, Pulsars, Relativity

Scientific paper

A new formula for gravitational-radiation energy loss that replaces the familiar quadrupole formula is presented. The new formula helps to clarify why the quadrupole formula works when it does. The origin of the correction tensor is discussed and then applied to the axially symmetric two-body problem. With the conventional equation of state, epsilon = epsilon(P), the correction tensor vanishes and the radiation is that of the bulk-motion quadrupole formula. An order-of-magnitude calculation is performed for a binary system, where it is found that there is the potential for contributions from nonlinear terms to be as significant as those from the linear terms after (Gm/alpha)exp- 5/6 orbits. This occurs after 100 years for the binary pulsar PSR 1913 + 16.

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