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Journal article
Gravitational Radiation from the Coalescence of Binary Neutron Stars: Effects Due to the Equation of State, Spin, and Mass Ratio
Physical review. D, Particles and fields, v 54(12), pp 7261-7277
17 Oct 1996
PMID: 10020743
Abstract
Phys.Rev.D54:7261-7277,1996 We calculate the gravitational radiation produced by the coalescence of
inspiraling binary neutron stars in the Newtonian regime using 3-dimensional
numerical simulations. 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. We
have run a number of simulations 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.
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Details
- Title
- Gravitational Radiation from the Coalescence of Binary Neutron Stars: Effects Due to the Equation of State, Spin, and Mass Ratio
- Creators
- Xing Zhuge - Drexel UniversityJoan M Centrella - Drexel UniversityStephen L. W McMillan - Drexel University
- Publication Details
- Physical review. D, Particles and fields, v 54(12), pp 7261-7277
- Publisher
- Cold Spring Harbor Press
- Resource Type
- Journal article
- Language
- English
- Academic Unit
- Physics
- Web of Science ID
- WOS:A1996WA83700020
- Scopus ID
- 2-s2.0-0000620229
- Other Identifier
- 991019170470904721
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Data related to this publication, from InCites Benchmarking & Analytics tool:
- Web of Science research areas
- Astronomy & Astrophysics
- Physics, Particles & Fields