论文标题
FRB 181112是二进制中子星合并后的快速旋转的巨大中子星？
FRB 181112 as a Rapidly-Rotating Massive Neutron Star just after a Binary Neutron Star Merger?: Implications for Future Constraints on Neutron Star Equations of State
论文作者
论文摘要
快速无线电爆发（FRB）181112的光曲线分为四个连续的脉冲，第一和第三脉冲之间的时间间隔（$ \ sim0.8 $ ms）与第二和第四脉冲之间的脉冲之间的时间间隔（$ \ sim0.8 $ ms）一致，这可以解释为在大约0.8美元的$ 0.8 $ MS时为中子星（NS）旋转。尽管此期间比当前已知的最快旋转的脉冲星（$ 1.4 $ MS）短，但对于二进制中子星（BNS）合并后立即形成的模拟大型NS是典型的。因此，如果周期性是真实的，则BNS合并是该FRB起源的好候选者。我们讨论如果从引力波（GW）同时从FRB中检测到这种周期性，则可以获得的未来含义。从FRB观察中推论的残余自旋周期$ p _ {\ rm rem} $是独特的信息，在合并后阶段，当前的GW观测值不易获得。如果与从GW数据中推断出的合并残余$ M _ {\ rm rem} $结合使用，它将对核物质状态方程式设置新约束。此外，合并后数量$ p _ {\ rm rem}/m _ {\ rm rem} $，或合并残留物的潮汐变形性与二进制潮汐可变形性参数$λ$在合并之前和frb-gw观察到新的$ limit of New Limit of New limit of New limit of the tidal tidal tidal tidal可变形性参数。因此，如果$λ$也通过GW数据很好地衡量，那么这两者之间的比较将为核物质和BNS合并的性质提供进一步的见解。
The light curve of the fast radio burst (FRB) 181112 is resolved into four successive pulses, and the time interval ($\sim0.8$ ms) between the first and third pulses coincides with that between the second and fourth pulses, which can be interpreted as a neutron star (NS) spinning at a period of about $0.8$ ms. Although this period is shorter than the most rapidly rotating pulsar currently known ($1.4$ ms), it is typical for a simulated massive NS formed immediately after the coalescence of binary neutron stars (BNS). Therefore, a BNS merger is a good candidate for the origin of this FRB if the periodicity is real. We discuss the future implications that can be obtained if such a periodicity is detected from FRBs simultaneously with gravitational waves (GW). The remnant spin period $P_{\rm rem}$ inferred from the FRB observation is unique information which is not readily obtained by current GW observations at the post-merger phase. If combined with the mass of the merger remnant $M_{\rm rem}$ inferred from GW data, it would set a new constraint on the equation of state of nuclear matter. Furthermore, the post-merger quantity $P_{\rm rem}/M_{\rm rem}$, or the tidal deformability of the merger remnant, is closely related to the binary tidal deformability parameter $Λ$ of NSs before they merge, and a joint FRB-GW observation will establish a new limit on $Λ$. Thus, if $Λ$ is also well measured by GW data, a comparison between these two will provide further insights into the nature of nuclear matter and BNS mergers.
