2006/11/17 by Masaru Shibata, Kōji Uryū, Koji Uryu · 9 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Gamma-ray bursts and supernovae #General relativity #Gravitational wave #Mathematical physics #Neutron star #Numerical relativity #Orbit (dynamics) #Physics #Pulsars and Gravitational Waves Research #RADIUS #Star (game theory) #astro-ph #gr-qc
paper · pdf · doi:10.1088/0264-9381/24/12/s09
published as Class.Quant.Grav.24:S125-S138,2007 · 14 pages. To appear in a special issue of Classical and Quantum Gravity: New Frontiers in Numerical Relativity
arxiv created 2006/11/17 · openalex publication_date 2007/05/30 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present our latest results for simulation for merger of black hole (BH)-neutron star (NS) binaries in full general relativity which is performed preparing a quasicircular state as initial condition. The BH is modeled by a moving puncture with no spin and the NS by the \Γ-law equation of state with \Γ=2 and corotating velocity field as a first step. The mass of the BH is chosen to be \≈ 3.2 M odot or 4.0M odot, and the rest-mass of the NS \≈ 1.4 M odot with relatively large radius of the NS \≈ 13--14 km. The NS is tidally disrupted near the innermost stable orbit but \∼ 80--90% of the material is swallowed into the BH and resulting disk mass is not very large as \∼ 0.3M odot even for small BH mass \∼ 3.2M odot. The result indicates that the system of a BH and a massive disk of \∼ M odot is not formed from nonspinning BH-NS binaries irrespective of BH mass, although a disk of mass \∼ 0.1M odot is a possible outcome for this relatively small BH mass range as \∼ 3--4M odot. Our results indicate that the merger of low-mass BH and NS may form a central engine of short-gamma-ray bursts.