Merger of black hole-neutron star binaries in full general relativity

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dc.creatorShibata, Masaru
dc.creatorUryu, Koji
dc.date2006-11-16
dc.date2006-11-17
dc.date.accessioned2026-07-07T10:36:35Z
dc.date.available2026-07-07T10:36:35Z
dc.descriptionWe 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 $\approx 3.2 M_{\odot}$ or $4.0M_{\odot}$, and the rest-mass of the NS $\approx 1.4 M_{\odot}$ with relatively large radius of the NS $\approx 13$--14 km. The NS is tidally disrupted near the innermost stable orbit but $\sim 80$--90% of the material is swallowed into the BH and resulting disk mass is not very large as $\sim 0.3M_{\odot}$ even for small BH mass $\sim 3.2M_{\odot}$. The result indicates that the system of a BH and a massive disk of $\sim M_{\odot}$ is not formed from nonspinning BH-NS binaries irrespective of BH mass, although a disk of mass $\sim 0.1M_{\odot}$ is a possible outcome for this relatively small BH mass range as $\sim 3$--4$M_{\odot}$. Our results indicate that the merger of low-mass BH and NS may form a central engine of short-gamma-ray bursts.
dc.description14 pages. To appear in a special issue of Classical and Quantum Gravity: New Frontiers in Numerical Relativity
dc.identifierhttps://arxiv.org/abs/astro-ph/0611522
dc.identifierhttp://arxiv.org/abs/astro-ph/0611522
dc.identifierClass.Quant.Grav.24:S125-S138,2007
dc.identifierdoi:10.1088/0264-9381/24/12/S09
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/180104
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleMerger of black hole-neutron star binaries in full general relativity
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