Gravitational Radiation from Coalescing Binary Neutron Stars
Xing Zhuge, Joan M. Centrella, and Stephen L. W. McMillan (Drexel, University)
TL;DR
This paper uses 3D numerical simulations to analyze gravitational waves from merging binary neutron stars, showing how wave spectra reveal details about neutron star properties and the equation of state.
Contribution
It introduces a simulation approach combining SPH and quadrupole approximation to study gravitational radiation from neutron star mergers, highlighting the spectrum's diagnostic potential.
Findings
Gravitational wave spectra contain detailed information about neutron star properties.
Simulations show the spectrum's sensitivity to the neutron star radius and equation of state.
Results suggest gravitational wave observations can infer neutron star internal physics.
Abstract
We calculate the gravitational radiation produced by the merger and coalescence of inspiraling binary neutron stars using 3-dimensional 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. We have run several simulations, varying both the neutron star radius and the equation of state. The resulting gravitational wave energy spectra are rich in information about the hydrodynamics of merger and coalescence. In particular, our results demonstrate that detailed information on both and the equation of state can in principle be extracted from the spectrum.
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