Measuring neutron star tidal deformability with Advanced LIGO: a Bayesian analysis of neutron star - black hole binary observations
Measuring neutron star tidal deformability with Advanced LIGO: a Bayesian analysis of neutron star - black hole binary observations
复制标题
使用高级 LIGO 测量中子星潮汐变形：中子星-黑洞双星观测的贝叶斯分析
DOI：
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发表时间：
2016
期刊：
影响因子：
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通讯作者：
H. Pfeiffer
中科院分区：
文献类型：
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作者：
Prayush Kumar;M. Purrer;H. Pfeiffer
先进的LIGO对引力波（GWs）的开创性发现将我们带入了观测GW天体物理学的时代。致密双星仍然是GW观测的主要目标源，其中中子星-黑洞（NSBH）双星是一个重要的子集。来自非黑洞黑洞源的GWs具有(a)中子星在吸入过程中被伴星黑洞潮汐扭曲的特征，以及(b)中子星在合并时潜在的潮汐破坏。在本文中，考虑到黑洞自旋的关键影响，我们提出了一种贝叶斯研究，利用对来自破坏性nshb合并的启发合并GW信号的观测，对中子星潮汐变形性ΛNS∝(R/M)NS5的可测量性进行了研究。首先，我们发现如果使用非潮汐模板来估计非潮汐信号的源参数，那么在估计非潮汐物理参数时引入的偏差只会对信噪比大于30的响亮信号产生显著影响。对于类似的大声信号，我们还发现我们可以开始对ΛNS（因子1-2）进行有趣的约束。接下来，我们将研究大量实际的非黑洞探测将如何改善我们对中子星潮汐变形性的测量。根据中子星状态方程，我们发现20-35个事件足以将ΛNS限制在±25%-50%的范围内。对于这些计算，我们假设LIGO将探测到质量在天体物理质量间隙内的黑洞。如果在LIGO探测到的NSBHs中仍然存在质量间隙，我们估计大约25%的额外探测将提供相当的ΛNS测量精度。在这两种情况下，我们发现最响亮的5-10个事件提供了大部分的潮汐信息，而不是数十个低信噪比事件的组合，从而有助于有针对性地进行非自然爆发事件的数值- gr跟踪。我们发现这些结果令人鼓舞，并建议在即将到来的LIGO-Virgo仪器观测nshb时计划测量ΛNS。
The pioneering discovery of gravitational waves (GWs) by Advanced LIGO has ushered us into an era of observational GW astrophysics. Compact binaries remain the primary target sources for GW observation, of which neutron star-black hole (NSBH) binaries form an important subset. GWs from NSBH sources carry signatures of (a) the tidal distortion of the neutron star by its companion black hole during inspiral, and (b) its potential tidal disruption near merger. In this paper, we present a Bayesian study of the measurability of neutron star tidal deformability ΛNS∝(R/M)NS5 using observation(s) of inspiral-merger GW signals from disruptive NSBH coalescences, taking into account the crucial effect of black hole spins. First, we find that if nontidal templates are used to estimate source parameters for an NSBH signal, the bias introduced in the estimation of nontidal physical parameters will only be significant for loud signals with signal-to-noise ratios greater than ≃30. For similarly loud signals, we also find that we can begin to put interesting constraints on ΛNS (factor of 1–2) with individual observations. Next, we study how a population of realistic NSBH detections will improve our measurement of neutron star tidal deformability. For an astrophysically likely population of disruptive NSBH coalescences, we find that 20–35 events are sufficient to constrain ΛNS within ±25%–50%, depending on the neutron star equation of state. For these calculations we assume that LIGO will detect black holes with masses within the astrophysical mass gap. In case the mass gap remains preserved in NSBHs detected by LIGO, we estimate that approximately 25% additional detections will furnish comparable ΛNS measurement accuracy. In both cases, we find that it is the loudest 5–10 events that provide most of the tidal information, and not the combination of tens of low-SNR events, thereby facilitating targeted numerical-GR follow-ups of NSBHs. We find these results encouraging, and recommend that an effort to measure ΛNS be planned for upcoming NSBH observations with the LIGO-Virgo instruments.
影响因子：
5
作者：
F. Pannarale;E. Berti;K. Kyutoku;B. Lackey;M. Shibata
通讯作者：
F. Pannarale;E. Berti;K. Kyutoku;B. Lackey;M. Shibata
影响因子：
4.9
作者：
Dominik, Michal;Berti, Emanuele;Pannarale, Francesco
通讯作者：
Pannarale, Francesco