Numerical relativity simulations of prompt collapse mergers: threshold mass and phenomenological constraints on neutron star properties after GW170817
Numerical relativity simulations of prompt collapse mergers: threshold mass and phenomenological constraints on neutron star properties after GW170817
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DOI：
10.1103/physrevd.105.103022
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发表时间：
2021-11
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通讯作者：
R. Kashyap;A. Das;D. Radice;Surendra Padamata;Aviral Prakash;D. Logoteta;A. Perego;D. Godzieba;S. Bernuzzi;I. Bombaci;F. J. Fattoyev;B. Reed;A. Schneider
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作者：
R. Kashyap;A. Das;D. Radice;Surendra Padamata;Aviral Prakash;D. Logoteta;A. Perego;D. Godzieba;S. Bernuzzi;I. Bombaci;F. J. Fattoyev;B. Reed;A. Schneider
我们使用一组新的 227 个数值相对论模拟确定等质量中子星 (NS) 合并中迅速（无反弹）黑洞形成的阈值质量。我们考虑了 23 个唯象和微观物理有限温度状态方程 (EOS)，包括具有超子和到解约束夸克的一阶相变的模型。我们确认阈值质量、阈值处的二元潮汐参数 (Λ th )、非旋转 NS 的最大质量和参考质量 NS 的半径之间存在 EOS 不敏感关系。我们结合 EOS 不敏感关系、NS 属性的现象学约束和 GW170817 的观测数据，得出改进的最大质量半径和 1.6 M (cid:12) NS 半径下限，分别为 9.81 km 和 10.90 km。我们还将 1.4 M (cid:12) NS 的半径和四极潮汐变形能力 (Λ) 分别限制为大于 10.74 km 和 172。我们在报告半径约束范围时考虑了所有独立参数的不确定性——拟合系数以及 GW170817 质量。我们讨论了一种使用未来 BNS 检测及其对即时或延迟塌陷的识别来限制 NS 最大质量上限和下限的方法。通过未来的观测，将有可能使用本工作中提出的方法对核密度及以上的物质特性得出更严格的约束。
We determine the threshold mass for prompt (no bounce) black hole formation in equal-mass neutron star (NS) mergers using a new set of 227 numerical relativity simulations. We consider 23 phenomenological and microphysical finite temperature equations of state (EOS), including models with hyperons and first-order phase transitions to deconfined quarks. We confirm the existence of EOS-insensitive relations between the threshold mass, the binary tidal parameter at the threshold (Λ th ), the maximum mass of nonrotating NSs, and the radii of reference mass NSs. We combine the EOS-insensitive relations, phenomenological constraints on NS properties and observational data from GW170817 to derive an improved lower limit on radii of maximum mass and 1.6 M (cid:12) NS of 9.81 km and 10.90 km, respectively. We also constrain the radius and quadrupolar tidal deformability (Λ) of a 1.4 M (cid:12) NS to be larger than 10.74 km and 172, respectively. We consider uncertainties in all independent parameters – fitting coefficients as well as GW170817 masses while reporting the range of radii constraints. We discuss an approach to constrain the upper as well as lower limit of NS maximum mass using future BNS detections and their identification as prompt or delayed collapse. With future observations it will be possible to derive even tighter constraints on the properties of matter at and above nuclear density using the method proposed in this work.