Matter imprints in waveform models for neutron star binaries: Tidal and self-spin effects
Matter imprints in waveform models for neutron star binaries: Tidal and self-spin effects
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DOI：
10.1103/physrevd.99.024029
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发表时间：
2018-04
影响因子：
5
通讯作者：
T. Dietrich;Sebastian Khan;R. Dudi;S. Kapadia;Prayush Kumar;A. Nagar;F. Ohme;F. Pannarale
中科院分区：
文献类型：
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作者：
T. Dietrich;Sebastian Khan;R. Dudi;S. Kapadia;Prayush Kumar;A. Nagar;F. Ohme;F. Pannarale
对两颗中子星合并产生的引力波和电磁波的联合观测标志着引力波多通道天文学(GWS)的开始。发展准确的引力波形模型是提取有关产生探测到的GW信号的二进制系统的性质的信息的关键前提。在双星中子星系统(BNS)中，潮汐效应也需要包含在建模中以获得准确的波形表示。在以前工作的基础上[Phys.Rev.D96,121501(2017)PRVDAQ2470-001010.1103/PhysRevD.96.121501]，我们探索了螺旋合并波形模型的性能，这些模型是通过在现有的非进动和进动二元黑洞系统的模型中添加一个基于数值相对论(NR)的相移部分近似值(NRTdal)来获得的，就像在LSC算法库套件中实现的那样。将得到的BNS波形与一组目标波形进行了比较和对比，这些目标波形是通过将NR波形(覆盖合并前的最后10个∼轨道并延伸到合并后阶段)与使用最先进的有效一体波模型从30赫兹计算的激励波形混合得到的。虽然由于目标波形的构建过程，在高级GW检测器可访问的整个频率范围内没有可用的误差预算，但波形集仅呈现真实信号的近似值。我们探讨了自旋项和NRTidal描述的结合对于获得相对于目标波形的最小失配(≲0.01)和相位差(≲1 rad)是必要的。我们还讨论了当前形式的NRTdal近似的可能的改进和缺陷。
The combined observation of gravitational and electromagnetic waves from the coalescence of two neutron stars marks the beginning of multimessenger astronomy with gravitational waves (GWs). The development of accurate gravitational waveform models is a crucial prerequisite to extract information about the properties of the binary system that generated a detected GW signal. In binary neutron star systems (BNS), tidal effects also need to be incorporated in the modeling for an accurate waveform representation. Building on previous work [Phys. Rev. D 96, 121501 (2017)PRVDAQ2470-001010.1103/PhysRevD.96.121501], we explore the performance of inspiral-merger waveform models that are obtained by adding a numerical relativity (NR) based approximant for the tidal part of the phasing (NRTidal) to existing models for nonprecessing and precessing binary black hole systems, as implemented in the LSC Algorithm Library Suite. The resulting BNS waveforms are compared and contrasted to a set of target waveforms which we obtain by hybridizing NR waveforms (covering the last ∼10 orbits up to the merger and extending through the postmerger phase) with inspiral waveforms calculated from 30 Hz obtained with a state-of-the-art effective-one-body waveform model. While due to the construction procedure of the target waveforms, there is no error budget available over the full frequency range accessible by advanced GW detectors, the waveform set presents only an approximation of the real signal. We probe that the combination of the self-spin terms and of the NRTidal description is necessary to obtain minimal mismatches (≲0.01) and phase differences (≲1 rad) with respect to the target waveforms. We also discuss possible improvements and drawbacks of the NRTidal approximant in its current form.