Gravitational Waves from the Merger of Binary Neutron Stars in a Fully General Relativistic Simulation

Details Gravitational Waves from the Merger of Binary Neutron Stars in a Fully General Relativistic Simulation Gravitational Waves from the Merger of Binary Neutron Stars in a Fully General Relativistic Simulation

2002-03-12

arxiv.org/abs/gr-qc/0203037v1

Prog.Theor.Phys. 107 (2002) 265

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

40 pages; pubslihed in Prog. Theor. Phys. 107 (2002), 265

Scientific paper

10.1143/PTP.107.265

We performed 3D numerical simulations of the merger of equal-mass binary neutron stars in full general relativity using a new large scale supercomputer. We take the typical grid size as (505,505,253) for (x,y,z) and the maximum grid size as (633,633,317). These grid numbers enable us to put the outer boundaries of the computational domain near the local wave zone and hence to calculate gravitational waveforms of good accuracy (within $\sim 10%$ error) for the first time. To model neutron stars, we adopt a $\Gamma$-law equation of state in the form $P=(\Gamma-1)\rho\epsilon$, where P, $\rho$, $\varep$ and $\Gamma$ are the pressure, rest mass density, specific internal energy, and adiabatic constant. It is found that gravitational waves in the merger stage have characteristic features that reflect the formed objects. In the case that a massive, transient neutron star is formed, its quasi-periodic oscillations are excited for a long duration, and this property is reflected clearly by the quasi-periodic nature of waveforms and the energy luminosity. In the case of black hole formation, the waveform and energy luminosity are likely damped after a short merger stage. However, a quasi-periodic oscillation can still be seen for a certain duration, because an oscillating transient massive object is formed during the merger. This duration depends strongly on the initial compactness of neutron stars and is reflected in the Fourier spectrum of gravitational waves. To confirm our results and to calibrate the accuracy of gravitational waveforms, we carried out a wide variety of test simulations, changing the resolution and size of the computational domain.

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