论文标题
在状态和哈勃常数的中子星程方程的多通间限制
Multi-messenger constraints on the neutron-star equation of state and the Hubble constant
论文作者
论文摘要
比原子核比原子核观察基于不同的使者（包括重力波和电磁信号）的中子恒星合并的观察结果，可用于研究物质密度的行为，并测量由哈勃常数描述的宇宙膨胀率。我们对重力波信号GW170817进行了联合分析，其电磁对应物AT2017GFO和GRB170817A，以及重力波信号GW190425，均起源于中子星级合并。我们使用X射线和无线电观察结果将它们与以前对脉冲星的测量结合在一起，以及使用手性有效野外理论来限制状态的中子星程方程的核理论计算。我们发现，$ 1.4 $太阳质量中子星的半径为$ 11.75^{+0.86} _ { - 0.81} \ \ rm km $ $ 90 \％$ $ pustrust，Hubble常数为$ 66.2^{+4.4} {+4.4} s^{ - 1} $ at $1σ$不确定性。
Observations of neutron-star mergers based on distinct messengers, including gravitational waves and electromagnetic signals, can be used to study the behavior of matter denser than an atomic nucleus, and to measure the expansion rate of the Universe described by the Hubble constant. We perform a joint analysis of the gravitational-wave signal GW170817 with its electromagnetic counterparts AT2017gfo and GRB170817A, and the gravitational-wave signal GW190425, both originating from neutron-star mergers. We combine these with previous measurements of pulsars using X-ray and radio observations, and nuclear-theory computations using chiral effective field theory to constrain the neutron-star equation of state. We find that the radius of a $1.4$ solar mass neutron star is $11.75^{+0.86}_{-0.81}\ \rm km$ at $90\%$ confidence and the Hubble constant is $66.2^{+4.4}_{-4.2}\ \rm km \,Mpc^{-1}\, s^{-1}$ at $1σ$ uncertainty.
