Constraining the p-Mode-g-Mode Tidal Instability with GW170817.
Constraining the p-Mode-g-Mode Tidal Instability with GW170817.
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用 GW170817 约束 p-Mode-g-Mode 潮汐不稳定性。
DOI：
10.1103/physrevlett.122.061104
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发表时间：
2019
影响因子：
8.6
通讯作者：
Abbott BP
中科院分区：
文献类型：
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作者：
Abbott BP
我们分析了一个建议的潮汐不稳定性耦合模式和中子星内部模式对GW170817的影响。这种非共振不稳定性将能量从双星轨道转移到恒星的内部模式，加速了螺旋驱动的引力波。我们模型的引力波信号的相位上使用三个参数，每星星的影响，这种不稳定性：一个整体的振幅，饱和频率，和光谱指数。排除这些额外的参数，我们计算贝叶斯因子（），将我们的模型与标准模型进行比较。我们发现，所观察到的信号是一致的波形模型，忽略effects，与（最大后验和90%的可信区域）。通过注入不包含效应的模拟信号并用模型恢复它们，我们表明即使在不存在效应的情况下也有可能获得类似的结果。我们发现中子星的振幅被限制在理论最大值的十分之几以下，最大值是这个最大值的十分之一和饱和频率的后线性。这表明，有不到几百个激发模式，假设他们都饱和波破碎。为了比较，理论上的上限dopstmodes饱和波破碎。因此，测量的约束条件只能排除参数的极值。它们还意味着不稳定性在整个螺旋上消散，即，只有不到百分之几的能量以引力波的形式辐射出去。
We analyze the impact of a proposed tidal instability couplingmodes andmodes within neutron stars on GW170817. This nonresonant instability transfers energy from the orbit of the binary to internal modes of the stars, accelerating the gravitational-wave driven inspiral. We model the impact of this instability on the phasing of the gravitational wave signal using three parameters per star: an overall amplitude, a saturation frequency, and a spectral index. Incorporating these additional parameters, we compute the Bayes factor () comparing ourmodel to a standard one. We find that the observed signal is consistent with waveform models that neglecteffects, with(maximuma posterioriand 90% credible region). By injecting simulated signals that do not includeeffects and recovering them with themodel, we show that there is aprobability of obtaining similareven wheneffects are absent. We find that theamplitude forneutron stars is constrained to less than a few tenths of the theoretical maximum, with maximaa posteriorinear one-tenth this maximum andsaturation frequency. This suggests that there are less than a few hundred excited modes, assuming they all saturate by wave breaking. For comparison, theoretical upper bounds suggestmodes saturate by wave breaking. Thus, the measured constraints only rule out extreme values of theparameters. They also imply that the instability dissipatesover the entire inspiral, i.e., less than a few percent of the energy radiated as gravitational waves.