发表机构
Universität Potsdam; Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（波茨坦大学; 马克斯·普朗克引力物理研究所（爱因斯坦研究所））
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究将慢旋转近似下的Love-Q准普适关系扩展至快速旋转中子星，通过显式考虑自旋并校准数值四极矩，将中位绝对百分比误差降低66%，为第三代引力波探测器波形建模提供更精确描述。
AI 中文摘要
双中子星并合的引力波观测通过波形上的有限尺寸效应探测中子星的状态方程。这些效应包括由于各自伴星引起的潮汐形变，但对于旋转中子星，还包括自旋引起的四极矩。通常，为避免引入额外的依赖于状态方程的参数，波形模型通过所谓的准普适关系将该四极矩与潮汐形变率联系起来。这些关系是在慢旋转近似下推导的，在较大自旋（即毫秒脉冲星）情况下变得不可靠。我们尝试通过显式考虑自旋来扩展现有的准普适关系，针对广泛的状态方程和自旋范围$0.15 \leq |\chi| \leq 0.6$，用数值计算的四极矩进行校准，并通过构造强制满足$\chi\rightarrow 0$极限。由此产生的自旋扩展关系在该范围内将相对于慢旋转关系的中位绝对百分比误差降低了66%。使用自旋扩展关系进行参数估计，在某些情况下减少了恢复的内在参数的偏差，尽管当考虑总体时，质量-自旋简并引起的偏差占主导。这些结果为旋转中子星双星的自旋诱导四极矩提供了更准确的描述，与第三代引力波探测器的波形建模相关。
英文摘要
Gravitational-wave observations of binary neutron star mergers probe the neutron star equation of state through finite-size effects on the waveform. These include the tidal deformation of the stars due to their respective companion, but for spinning neutron stars also include the spin-induced quadrupole moment of the stars. Typically, to avoid introducing additional equation of state dependent parameters, waveform models relate this quadrupole moment to the tidal deformability through so-called quasi-universal relations. These are derived under the slow-rotation approximation, which at larger spins, i.e., for millisecond pulsars, becomes unreliable. We attempt to extend the existing quasi-universal relations by explicitly accounting for the spin, calibrating it against numerically computed quadrupole moments across a broad set of equations of state and spins $0.15 \leq |χ| \leq 0.6$ with the $χ\rightarrow 0$ limit enforced by construction. The resulting spin-extended relation reduces the median absolute percentage error relative to the slow-rotation relation by 66\% across this range. Parameter estimation using the spin-extended relation reduces biases in recovered intrinsic parameters in some cases, though biases from mass-spin degeneracies dominate largely when a population is considered. These results provide a more accurate description of the spin-induced quadrupole moment for spinning neutron star binaries, relevant for waveform modelling with third-generation gravitational-wave detectors.
Comments16 pages, 9 figures
