2014/05/31 by Koutarou Kyutoku, Masaru Shibata, Keisuke Taniguchi · 1 citation
Earth and Planetary Sciences · Mathematics · Physics and Astronomy · #Angular velocity #Astronomy #Astrophysics #Binary number #Binary star #Classical mechanics #Eccentricity (behavior) #Gamma-ray bursts and supernovae #Geophysics and Gravity Measurements #Hydrostatic equilibrium #Mass ratio #Mathematics #Neutron star #Orbital eccentricity #Orbital elements #Orbital mechanics #Orbital speed #Physics #Pulsars and Gravitational Waves Research #Satellite #Stars #astro-ph.HE #gr-qc
paper · pdf · doi:10.1103/physrevd.90.064006
published as Phys. Rev. D 90, 064006 (2014) · 20 pages, 12 figures, matched to the published version
arxiv created 2014/09/03 · openalex publication_date 2014/09/03 · arxiv updated 2017/12/27 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We develop a method to compute low-eccentricity initial data of binary neutron stars required to perform realistic simulations in numerical relativity. The orbital eccentricity is controlled by adjusting the orbital angular velocity of a binary and incorporating an approaching relative velocity of the neutron stars. These modifications improve the solution primarily through the hydrostatic equilibrium equation for the binary initial data. The orbital angular velocity and approaching velocity of initial data are updated iteratively by performing time evolutions over \ensuremath∼3 orbits. We find that the eccentricity can be reduced by an order of magnitude compared to standard quasicircular initial data, specifically from \ensuremath∼0.01 to \ensuremath\lesssim0.001, by three successive iterations for equal-mass binaries leaving \ensuremath∼10 orbits before the merger.