Physics
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aps..may..a902c&link_type=abstract
American Physical Society, APS/AAPT Joint Meeting, May 2-5, 1996, abstract #A9.02
Physics
Scientific paper
We calculate the gravitational radiation produced by the coalescence of inspiraling binary neutron stars using 3-dimensional numerical simulations. The stars are initially modeled as polytropes and start out on circular orbits 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. To cause the stars to spiral in, we mimic the effects of gravitational radiation reaction by introducing a frictional term into the equations of motion to remove orbital energy at the rate given by the equivalent point-mass inspiral. As the neutron stars get closer together the tidal distortions grow and eventually dominate, and coalescence quickly follows. We have run simulations varying the equation of state, radius, spin, and mass ratio of the stars, and we explore the effects of these parameters on the resulting gravitational wave energy spectrum. This research is supported by NSF grant PHY--9208914, and the simulations were carried out at the Pittsburgh Supercomputing Center.
Centrella Joan M.
McMillan Stephen L. W.
Zhuge Xing
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