1999/11/11 by Grant J. Mathews, G. J. Mathews, J. R. Wilson · 3 citations
Mathematics · Physics and Astronomy · #Angular momentum #Astrophysical Phenomena and Observations #Astrophysics #Binary number #Classical mechanics #Compressibility #Compression (physics) #Conservative vector field #Gamma-ray bursts and supernovae #Mathematics #Mechanics #Neutron star #Orbit (dynamics) #Orbital motion #Physics #Pulsars and Gravitational Waves Research #gr-qc
paper · pdf · doi:10.1103/physrevd.61.127304
published as Phys.Rev. D61 (2000) 127304 · Submitted to Phys. Rev. D
arxiv created 1999/11/11 · openalex publication_date 2000/05/24 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We report on numerical results from a revised hydrodynamic simulation of binary neutron-star orbits near merger. We find that the correction recently identified by Flanagan significantly reduces but does not eliminate the neutron-star compression effect. Although results of the revised simulations show that the compression is reduced for a given total orbital angular momentum, the inner most stable circular orbit moves to closer separation distances. At these closer orbits significant compression and even collapse are still possible prior to merger for a sufficiently soft EOS. We note, however, that the compression observed in the simulation is within the numerical error and also of order of the error expected from the approximation of a conformally flat spatial three metric. The reduced compression in the corrected simulation is consistent with other recent studies of rigid irrotational binaries in quasiequilibrium in which the compression effect is observed to be small. Another significant effect of this correction is that the derived binary orbital frequencies are now in closer agreement with post-Newtonian expectations.