Gravitational radiation from coalescing binary neutron stars.

Details Gravitational radiation from coalescing binary neutron stars. Gravitational radiation from coalescing binary neutron stars.

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994phrvd..50.6247x&link_type=abstract

Physical Review D, Vol. 50, No. 10, p. 6247 - 6261

Physics

56

Close Binaries: Coalescence, Close Binaries: Neutron Stars, Close Binaries: Gravitational Radiation

Scientific paper

The authors calculate the gravitational radiation produced by the merger and coalescence of inspiraling binary neutron stars using 3D numerical simulations. The stars are modeled as polytropes and start out in the point mass limit at wide separation. The hydrodynamic integration is performed using smooth particle hydrodynamics (SPH) with Newtonian gravity, and the gravitational radiation is calculated using the quadrupole approximation. The authors have run several simulations, varying both the neutron star radius and the equation of state. The resulting gravitational wave energy spectra dE/df are rich in information about the hydrodynamics of merger and coalescence. In particular, the results demonstrate that detailed information on both GM/Rc2 and the equation of state can in principle be extracted from the spectrum.

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