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We calculate the gravitational radiation produced by the coalescence ofinspiraling binary neutron stars in the Newtonian regime using 3-dimensionalnumerical simulations. The stars are modeled as polytropes and start out in thepoint-mass regime at wide separation. The hydrodynamic integration is performedusing smooth particle hydrodynamics (SPH) with Newtonian gravity, and thegravitational radiation is calculated using the quadrupole approximation. Wehave run a number of simulations varying the neutron star radii, equations ofstate, spins, and mass ratio. The resulting gravitational waveforms and spectraare rich in information about the hydrodynamics of coalescence, and showcharacteristic dependence on GM/Rc^2, the equation of state, and the massratio.Comment: 39 pages, uses Latex 2.09. To be published in the Dec. 15, 1996 issue  of Physical Review D. 16 Figures (bitmapped). Originals available in  compressed Postscript format at ftp://zonker.drexel.edu/papers/PAPER2

Gravitational radiation from the coalescence of binary neutron stars: Effects due to the equation of state, spin, and mass ratio