Simulating coalescing compact binaries by a new code (SACRA)

Abstract

We report our new code (named SACRA) for numerical relativity simulations in which an adaptive mesh refinement algorithm is implemented. In this code, the Einstein equations are solved in the BSSN formalism with a fourth-order finite differencing, and the hydrodynamic equations are solved by a third-order high-resolution central scheme. The fourth-order Runge-Kutta scheme is adopted for integration in time. To test the code, simulations for coalescence of black hole-black hole (BH-BH), neutron star-neutron star (NS-NS), and black hole-neutron star (BH-NS) binaries are performed, and also, properties of BHs formed after the merger and gravitational waveforms are compared among those three cases. For the simulations of BH-BH binaries, we adopt the same initial conditions as those by Buonanno et al. [Phys. Rev. D 75, 124018 (2007)] and compare numerical results. We find reasonable agreement except for a slight disagreement possibly associated with the difference in choice of gauge conditions and numerical schemes. For an NS-NS binary, we performed simulations employing both SACRA and Shibata's previous code, and find reasonable agreement between two numerical results for the final outcome and qualitative property of gravitational waveforms. We also find that the convergence is relatively slow for numerical results of NS-NS binaries, and again realize that longterm numerical simulations with several resolutions and grid settings are required for validating the results. For a BH-NS binary, we compare numerical results with our previous ones, and find that gravitational waveforms and properties of the BH formed after the merger agree well with those of our previous ones, although the disk mass formed after the merger is less than 0.1% of the total rest mass, which disagrees with the previous result. We also report numerical results of a longterm simulation (with ∼ 4 orbits) for a BH-NS binary for the first time. All these numerical results show behavior of convergence, and extrapolated numerical results for time spent in the inspiral phase agree with post-Newtonian predictions in a reasonable accuracy. These facts validate the results by SACRA.

Anisotropic mass ejection from black hole-neutron star binaries: Diversity of electromagnetic counterparts

“…Our simulations are performed in full general relativity with an adaptive-mesh-refinement code, SACRA [24]. Improvements to previous simulations are summarized as follows (see also [18]).…”

Detectable radio flares following gravitational waves from mergers of binary neutron stars

“…Some (e.g., Rosswog et al 2000;Ruffert & Janka 2001;Rosswog & Price 2007) use Newtonian dynamics (modified to allow for gravitational radiation back-reaction) with detailed microphysics. Others (e.g., Yamamoto et al 2008;Rezzolla et al 2010) use full General relativistic dynamics with different levels of approximate microphysics, with or without MHD. In almost all NS 2 simulations one finds an accretion disk surrounding a rapidly rotating massive object that eventually collapses to a black hole.…”

Three-dimensional evolution of differentially rotating magnetized neutron stars

“…For the theoretical studies of the BNS mergers, numerical relativity is the unique and robust approach. A number of numerical simulations have been performed [3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19] since the first success in 2000 [20].…”