Gravitational radiation from pairs of realistic, nonaccreting compact stars

Details Gravitational radiation from pairs of realistic, nonaccreting compact stars Gravitational radiation from pairs of realistic, nonaccreting compact stars

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...431..254s&link_type=abstract

The Astrophysical Journal, Part 1, vol. 431, no. 1, p. 254-263

Statistics

Computation

2

Binary Stars, Gravitational Waves, Stellar Evolution, Stellar Interiors, Stellar Luminosity, Stellar Mass, Computational Astrophysics, Magnetic Fields, Relativity, Stellar Mass Accretion

Scientific paper

The dependence is described of the gravitational-radiation luminosity on the changing internal characteristics of the members of a binary system which are assumed to be realistic compact stars. The new, general relativistic post-Newtonian contribution to the gravitational-radiation luminosity is due to the evolution of the nonaccreting members of the stellar pair, and it is nonvanishing even in the case of equal inertial masses of the members. For nonaccreting members of equal inertial masses in circular relative motion, the rate of emission of gravitational radiation due to the change of the members' internal characteristics is the same for both kinds of change, namely deceleration or acceleration of the axial rotations, and/or increase or decrease of the radii. In this case the value of the emission rate although generally small, can be comparable to the corresponding purely orbital one of the same post-Newtonian order. Also the dependence of the gravitational-wave phase change on the changing internal characteristics is examined and is compared with that due to simply orbital, Newtonian, or post-Newtonian characteristics. Finally, the underlying theoretical framework permits an analogous investigation for different inertial masses and, in principle, also for mass-accreting binaries.

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