发表机构
Université Paris Cité, CNRS, Astroparticule et Cosmologie（巴黎西岱大学，法国国家科学研究中心，基本粒子与宇宙学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究在4PN阶精度下，通过摄动分析结合EFT哈密顿量形式，计算了任意质量比自旋致密双星的ISCO稳定性判据，结果与GSF计算吻合良好，还对比了MPD方程预测并讨论共旋黑洞双星的ISCO。
AI 中文摘要
我们计算了四阶后牛顿（4PN）阶精度下，轨道角动量自旋取向任意质量比致密双星的最内稳定圆轨道（ISCO）的规范不变稳定性判据。该计算为摄动分析，纳入了自旋-轨道耦合与自旋-自旋耦合贡献，二者均达次-次-领头阶，以及领头阶的三阶和四阶自旋贡献，所有这些均是在有效场论（EFT）哈密顿量形式框架内的前期工作中计算得到的。在测试粒子极限下，我们恢复了截断至4PN阶精度的克尔（Kerr）黑洞ISCO。通过一阶质量比估计ISCO偏移，并将结果与数值引力自作用力（GSF）计算结果对比，发现对于逆行自旋（最大逆行自旋时偏差最小）和中等程度顺行自旋，二者吻合良好。对于近最大顺行自旋，由于其接近黑洞（BH）视界，后牛顿（PN）方法无法确定ISCO。我们还估计了测试粒子自旋引起的ISCO偏移，并将结果与描述自旋粒子绕克尔黑洞运动的马蒂松-帕帕佩特罗-迪克森（MPD）方程的精确预测进行对比。最后，我们讨论了共旋黑洞双星的稳定性及ISCO。
英文摘要
We compute, up to 4th post-Newtonian (4PN) order, the gauge-invariant stability criterion determining the innermost stable circular orbit (ISCO) for arbitrary-mass compact binaries with spins aligned with the orbital angular momentum. Our calculation, a perturbation analysis, incorporates spin-orbit and spin-spin contributions, both up to next-to-next-to-leading order, as well as leading-order cubic and quartic spin contributions, all calculated in prior works within the effective-field-theory (EFT) Hamiltonian formalism. In the test-mass limit, we recover the Kerr ISCO truncated at 4PN order. Estimating the ISCO shift at first order in the mass ratio and comparing our results with numerical gravitational self-force (GSF) calculations, we find good agreement for retrograde spin (the smallest discrepancy being obtained for maximal retrograde spin) and moderate prograde spin. For nearly maximal prograde spin, the PN approach fails to determine the ISCO, for it is close to the black hole (BH) horizon. We also estimate the ISCO shift due to the test-particle spin and compare our result with the exact prediction from the Mathisson-Papapetrou-Dixon (MPD) equations for a spinning particle orbiting a Kerr black hole. Finally, we discuss the stability and the ISCO of corotating black-hole binaries.
Comments30 pages, 5 figures
