Equation of state of dense matter in the multimessenger era
Equation of state of dense matter in the multimessenger era
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DOI：
10.1103/physrevd.99.121301
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发表时间：
2019-01
影响因子：
5
通讯作者：
Ying Zhou;Lie-Wen Chen;Zhen Zhang
中科院分区：
文献类型：
--
作者：
Ying Zhou;Lie-Wen Chen;Zhen Zhang
虽然对称核物质（SNM）在过饱和密度下的态方程（EOS）已经相对较好地受到重离子碰撞的约束，但由于对称能的高密度行为知之甚少，高密度富中子物质的态方程在很大程度上仍然是不确定的。利用重离子碰撞的超饱和密度下SNM的EOS约束，结合电磁观测的有限核数据和$2M_\odot$中子星的存在，我们证明了高密度对称能不能太软，这导致了$1.4M_\odot$中子星的无因次潮汐变形能力$\Lambda_{1.4} \ge 193$和半径$R_{1.4} \ge 11.1$ km的下界。此外，我们发现LIGO和室女座合作组织从双中子星合并中探测到的引力波信号GW170817最近对$\Lambda_{1.4} \le 580$的约束排除了过于坚硬的高密度对称能，导致其上限为$R_{1.4} \le 13.3$ km。EM和引力测量共同对SNM、纯中子物质和中子星物质的高密度对称能和EOS施加了严格的约束。
While the equation of state (EOS) of symmetric nuclear matter (SNM) at suprasaturation densities has been relatively well constrained from heavy-ion collisions, the EOS of high-density neutron-rich matter is still largely uncertain due to the poorly known high-density behavior of the symmetry energy. Using the constraints on the EOS of SNM at suprasaturation densities from heavy-ion collisions together with the data of finite nuclei and the existence of $2M_\odot$ neutron stars from electromagnetic (EM) observations, we show that the high-density symmetry energy cannot be too soft, which leads to lower bounds on dimensionless tidal deformability of $\Lambda_{1.4} \ge 193$ and radius of $R_{1.4} \ge 11.1$ km for $1.4M_\odot$ neutron star. Furthermore, we find that the recent constraint of $\Lambda_{1.4} \le 580$ from the gravitational wave signal GW170817 detected from the binary neutron star merger by the LIGO and Virgo Collaborations rules out too stiff high-density symmetry energy, leading to an upper limit of $R_{1.4} \le 13.3$ km. All these terrestrial nuclear experiments and astrophysical observations based on strong, EM and gravitational measurements together put stringent constraints on the high-density symmetry energy and the EOS of SNM, pure neutron matter and neutron star matter.