论文标题
GW190814中次要物体作为中子星的可能性
The possibility of the secondary object in GW190814 as a neutron star
论文作者
论文摘要
GW190814中的Ligo Scientific and Pirgo合作（LVC）观察到了一个紧凑的物体，质量为$ 2.50-2.67〜M_ \ odot $，这为对核核问题的调查提供了巨大的挑战。为了研究该对象，中子星的性质是在最新密度依赖性相对论均值场（DDRMF）参数化中系统计算的，该参数由球形核的基态特性确定。由DD-MEX和DD-LZ1组计算出的中子星的最大质量的最大质量约为$ 2.55〜M_ \ ODOT $，其状态的较硬方程是由高密度下的向量电位产生的强烈反击贡献。它们的最大声音$ C_S/C $小于Neutron Star中心的$ \ sqrt {0.8} $，而无尺寸的潮汐变形可为$ 1.4〜m_ \ odot $小于$ 800 $。此外，$ 1.4〜m_ \ odot $的半径也满足了观察到质量 - 拉迪乌斯同时测量的限制（更加良好）。因此，我们得出的结论是，人们不能排除GW190814中二级对象作为由DDRMF模型的强子物质组成的中子恒星的可能性。
A compact object was observed with a mass $2.50-2.67~M_\odot$ by LIGO Scientific and Virgo collaborations (LVC) in GW190814, which provides a great challenge to the investigations into the supranuclear matter. To study this object, properties of neutron star are systematically calculated within the latest density-dependent relativistic mean-field (DDRMF) parameterizations, which are determined by the ground state properties of spherical nuclei. The maximum masses of neutron star calculated by DD-MEX and DD-LZ1 sets can be around $2.55~M_\odot$ with quite stiff equations of state generated by their strong repulsive contributions from vector potentials at high densities. Their maximum speeds of sound $c_s/c$ are smaller than $\sqrt{0.8}$ at the center of neutron star and the dimensionless tidal deformabilities at $1.4~M_\odot$ are less than $800$. Furthermore, the radii of $1.4 ~M_\odot$ also satisfy the constraint from the observation of mass-radius simultaneous measurements (NICER). Therefore, we conclude that one cannot exclude the possibility of the secondary object in GW190814 as a neutron star composed of hadron matter from DDRMF models.
