Numerical Models of Binary Neutron Star System Mergers. II. Coalescing Models with Post-Newtonian Radiation Reaction Forces

Details Numerical Models of Binary Neutron Star System Mergers. II. Coalescing Models with Post-Newtonian Radiation Reaction Forces Numerical Models of Binary Neutron Star System Mergers. II. Coalescing Models with Post-Newtonian Radiation Reaction Forces

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...570..303c&link_type=abstract

The Astrophysical Journal, Volume 570, Issue 1, pp. 303-313.

Astronomy and Astrophysics

Astronomy

2

Gravitation, Gravitational Waves, Hydrodynamics, Relativity, Stars: Neutron

Scientific paper

Using a grid-based staggered-mesh hydrodynamics code, we present the evolution of initially Newtonian equilibrium configurations of symmetric binary neutron star systems under the influence of a post-Newtonian gravitational radiation reaction potential. These simulations indicate that the time to merger for binaries with separations on the order of a few stellar radii is between 1/2 and 1 Keplerian period of the initial configuration. These results are in contrast to the larger timescales calculated from earlier smoothed particle hydrodynamics calculations that include quadrupolar-type radiation reaction forces. The implications of our studies are discussed in the context of observable effects on the gravitational waveforms expected to be observed by ground-based gravity-wave detectors such as the Laser Interferometer Gravitational-Wave Observatory and the restrictions placed on the choice of initial data for fully relativistic calculations.

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