Merger of black hole and neutron star in general relativity
Some of the latest results of the simulation for the merger of black hole (BH)-neutron star (NS) binaries in full general relativity is presented. As the initial condition, we prepare a quasicircular state in which the BH is modeled by a moving puncture with no spin. The Γ-law equation of state with Γ=2 and irrotational velocity field are used for modeling the NS. The BH mass is chosen to be≈4M??, whereas the rest-mass of the NS is≈ 1.4M?? and the radius is≈13km. The NS is tidally disrupted near the innermost stable orbit but more than～90％ of the material is quickly swallowed into the BH and the resultant disk mass is≈0.1M??. The thermal energy of the material in the disk increases by the shock heating occurred in the collision between the spiral arms. Our results indicate that the merger between a low-mass BH and its companion NS may form a central engine of short-gamma-ray bursts. Gravitational waveforms are also presented. We find that the amplitude of gravitational waves quickly decreases after the tidal disruption and the amplitude of the quasinormal mode ringing is small.
black hole neutron star gravitational waves
Masaru Shibata Keisuke Taniguchi Koji Uryu
Graduate School of Arts and Sciences, University of Tokyo, Komaba, Tokyo 153-8902, Japan Department of Physics, University of Illinois at Urbana-Champaign, Illinois 61801, USA Department of Physics and Earth Sciences, University of the Ruykyus, Okinawa 903-0213, Japan
国际会议
紧凑型物体的天体物理学国际会议(International Conference on Astrophysics of Compact Objects)
安徽黄山
英文
297-306
2007-07-01（万方平台首次上网日期，不代表论文的发表时间）