Numerical-relativity studies for coalescing binary neutron stars and black hole-neutron star binaries

在中子星状态方程、中子星质量和黑洞质量以及黑洞自旋范围的不同条件下，对中子星双子星和黑洞-中子星双子星合并进行了数值相对论模拟。我们定量、系统地阐明了这些双星的并合过程、并合后形成的产物以及发出的引力波。特别是，我们澄清了合并阶段的引力波强烈依赖于中子星和黑洞自旋的状态方程。这意味着它们将能够受到引力波探测的限制，这将在不久的将来由引力波探测器实现。

Numerical-relativity simulations for the coalescence of binary neutron stars and black hole-neutron star binaries were performed for a wide variety of neutron star’s equations of state, for a wide range of masses of neutron stars and black holes, and fora wide range of black hole spins. We quantitatively and systematically clarified the merger process of these binaries, the product formed after the merger, and gravitational waves emitted. In particular, we clarified that gravitational waves in the merger phase depend strongly on the equations of state of neutron stars and black hole spins. This implies that they will be able to be constrained by the detection of gravitational waves which will be achieved in the near future by gravitational-wave detectors.