Yukawa Institute for Theoretical Physics, Kyoto University, Japan.
Phys Rev Lett. 2011 Nov 18;107(21):211101. doi: 10.1103/PhysRevLett.107.211101.
Numerical simulations for the merger of binary neutron stars are performed in full general relativity incorporating both nucleonic and hyperonic finite-temperature equations of state (EOS) and neutrino cooling. It is found that even for the hyperonic EOS, a hypermassive neutron star is first formed after the merger for the typical total mass ≈2.7M(⊙), and subsequently collapses to a black hole (BH). It is shown that hyperons play a substantial role in the postmerger dynamics, torus formation around the BH, and emission of gravitational waves (GWs). In particular, the existence of hyperons is imprinted in GWs. Therefore, GW observations will provide a potential opportunity to explore the composition of neutron star matter.
在包含核子和超子有限温物态方程和中微子冷却的全广义相对论框架下，对双中子星并合进行了数值模拟。研究发现，即使对于超子物态方程，对于典型的总质量 ≈2.7M(⊙)，在并合之后也首先形成一颗超重中子星，随后它会塌缩成一个黑洞。结果表明，超子在并合后的动力学、黑洞周围的环形成以及引力波（GW）的发射中起了重要作用。特别是，超子的存在在 GW 中留下了印记。因此，GW 观测将为探索中子星物质的组成提供一个潜在的机会。
