论文标题
二进制内部星形标准GW170817和GW190425的后续分析使用牛顿后波形模型
Follow-up analyses of the binary-neutron-star signals GW170817 and GW190425 by using post-Newtonian waveform models
论文作者
论文摘要
我们重新分析了二进制内部恒星信号GW170817和GW190425，重点关注Inspiral Segime，以避免在启动后验证方面的波形建模不确定性。我们将牛顿后波形模型用作模板，在理论上是僵化且有效地描述了灵感制度的模板。我们通过对点粒子动力学和潮汐效应使用不同的描述来研究二进制潮汐变形性$ \tildeλ$估计的潜在系统差异。我们发现，当使用相同的潮汐模型时，$ \tildeλ$的估计值在点粒子部分的三个模型之间没有明显的系统差异：TF2，TF2G和TF2+。我们比较了潮汐阶段中不同后牛顿后命令给出的不同潮汐描述。我们的结果表明，$ \tildeλ$的估计值略微取决于潮汐阶段的牛顿后顺序，而潮汐后北顿订单的增加并不会导致$ \tildeλ$的估算值的单调变化。我们还比较了纽约后潮汐模型和数值估计式潮汐模型获得的$ \tildeλ$的估计。我们发现，牛顿后模型的估计值略大于$ \tildeλ$，而后验分布较大，而后验分布比数值估计的模型更大。根据贝叶斯模型比较，很难通过依靠GW170817和GW190425数据来确定牛顿后订单之间的偏好。我们的结果表明，在牛顿后模型中，数值循环模型之间没有偏好。此外，我们对Newtonian模型的中子星的等式模型提出了约束，该模型表明，GW170817数据数据不足的模型较少，尽管它们的约束略弱于数值估计性校准的潮汐模型。
We reanalyze the binary-neutron-star signals, GW170817 and GW190425, focusing on the inspiral regime to avoid uncertainties on waveform modeling in the postinspiral regime. We use post-Newtonian waveform models as templates, which are theoretically rigid and efficiently describe the inspiral regime. We study potential systematic difference in estimates of the binary tidal deformability $\tildeΛ$ by using different descriptions for the point-particle dynamics and tidal effects. We find that the estimates of $\tildeΛ$ show no significant systematic difference among three models for the point-particle parts: TF2, TF2g, and TF2+, when they employ the same tidal model. We compare different tidal descriptions given by different post-Newtonian orders in the tidal phase. Our results indicate that the estimates of $\tildeΛ$ slightly depend on the post-Newtonian order in the tidal phase and an increase in the tidal post-Newtonian order does not lead to a monotonic change in the estimate of $\tildeΛ$. We also compare the estimate of $\tildeΛ$ obtained by the post-Newtonian tidal model and numerical-relativity calibrated tidal models. We find that the post-Newtonian model gives slightly larger estimate of $\tildeΛ$ and wider posterior distribution than the numerical-relativity calibrated models. According to Bayesian model comparison, it is difficult to identify a preference among the post-Newtonian orders by relying on the GW170817 and GW190425 data. Our results indicate no preference among numerical-relativity calibrated tidal models over the post-Newtonian model. Additionally, we present constraints on equation-of-state models for neutron stars with the post-Newtonian model, which show that the GW170817 data disfavor less compact models, though they are slightly weaker constraints than the numerical-relativity calibrated tidal models.
