Merger of black hole-neutron star binaries: Nonspinning black hole case

Abstract

We perform a simulation for merger of a black hole (BH)-neutron star (NS) binary in full general relativity 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. Corotating velocity field is assumed for the NS. The mass of the BH and the rest-mass of the NS are chosen to be ≈ 3.2M⊙ and ≈ 1.4M⊙ with relatively large radius of the NS ≈ 14 km. The NS is tidally disrupted near the innermost stable orbit but ∼ 80% of the material is swallowed into the BH with small disk mass ∼ 0.3M⊙ even for such small BH mass ∼ 3M⊙. The result indicates that the system of a BH and a massive disk of ∼ M⊙ is not formed from nonspinning BH-NS binaries, although a disk of mass ∼ 0.1M⊙ is a possible outcome.

Search for Gravitational-Wave Bursts Associated With Gamma-Ray Bursts Using Data From Ligo Science Run 5 and Virgo Science Run 1

“…Preliminary explorations of the impact of magnetic fields have also been made by Anderson et al (2008), Liu et al (2008), and Giacomazzo et al (2009). The mergers of black-hole-neutronstar binaries have been studied by Shibata & Uryū (2006), Shibata & Uryū (2007), , Etienne et al (2008), Duez et al (2008), Yamamoto et al (2008), Shibata et al (2009), Etienne et al (2009), andDuez et al (2010). For other progenitor types, particularly for long GRBs, there are no robust models for the gravitational-wave emission (see, for example, Fryer et al 2002;Kobayashi & Meszaros 2003;van Putten et al 2004;Ott 2009 for possible scenarios).…”

Simulating binary neutron stars: Dynamics and gravitational waves

“…To date, work on black hole-neutron star binaries has been limited to a few cases [19,20,21]. As a result, our understanding of this type of system is still in its infancy.…”

Relativistic hydrodynamics in the presence of puncture black holes

“…We now plan to adopt the puncture method to simulate BHNS binaries fully self-consistently, similar to the calculations of [45,46]. In contrast to [45,46], we plan to evolve quasiequilibrium conformal thin-sandwich initial data. This poses the conceptional problem that the initial data use excision to model the BH, while the dynamical evolution requires initial data everywhere.…”

“…In fact, this is the approach adopted in the only fully self-consistent dynamical simulations of orbiting BHNS binaries to date [45,46] (see [47,48,49,50] for other preliminary relativistic simulations of BHNS binaries, and [51,52] for discussion about and simulations of alternate configurations without the use of excision).…”