Physics
Scientific paper
Apr 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aps..apr..j403c&link_type=abstract
American Physical Society, APS/AAPT Joint Meeting, April 18-21, 1997, abstract #J4.03
Physics
Scientific paper
Coalescing binary neutron stars are among the most promising sources for detection by gravitational wave interferometers such as LIGO, VIRGO, and GEO. The inspiral phase comprises the last several thousand binary orbits and covers the frequency range f ~ 10--1000 Hz. During this stage, the separation of the stars is much larger than their radii and the gravitational radiation can be calculated using post-Newtonian expansions in the point-mass limit. Analysis of the inspiral wave forms is expected to reveal the masses and spins of the neutron stars, as well as the orbital parameters of the binary systems. When the binary separation is comparable to the neutron star radius, hydrodynamic effects become dominant and coalescence takes place within a few orbits. Three-dimensional numerical simulations are needed to study the detailed hydrodynamical evolution of the coalescence. This talk will discuss calculations of the gravitational radiation produced by the coalescence of binary neutron stars. The main focus will be on recent simulations carried out in the Newtonian regime. In these calculations, the stars are modeled as polytropes and start out in the point-mass regime 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. A number of simulations have been run, varying the neutron star radii, equations of state, spins, and mass ratio. The resulting gravitational waveforms and spectra are rich in information about the hydrodynamics of coalescence, and show characteristic dependence on GM/Rc^2, the equation of state, and the mass ratio. In addition, current work on simulations incorporating full general relativity will be discussed.
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