银河核中大质量黑洞三重态的后牛顿演化：I.数值实现与测试
Post-Newtonian Evolution of Massive Black Hole Triplets in Galactic Nuclei: I. Numerical Implementation and Tests
摘要：
大质量黑洞双星（MBHB）被认为是低频域引力波（GW）的主要来源，正在进行和即将进行的脉冲星定时阵列活动和未来的星载任务，如{ \it eLISA}。然而，在现实的天体物理环境中，许多低红移的MBHB可能无法达到足够小的分离，以允许显着的GW排放，而是在（子）pc尺度轨道上失速。这个“最后秒差距问题”可以通过第三个大质量黑洞（MBH）--“入侵者”--的出现得到缓解，在某些条件下，它的作用可以迫使内部的MBHB在一个非常偏心的轨道上，从而允许强烈的GW发射，最终导致合并。详细评估的过程中，最终驱动的诱导Kozai-Lidov振荡的MBHB轨道，需要一个广义相对论的治疗和列入外部因素，如牛顿进动的入侵者轨道在银河系的潜力和硬化散射了背景恒星。为了解决这个问题，我们开发了一个三体后牛顿（PN）代码框架中的一个现实的银河系的潜力，包括非耗散1 PN和2 PN条款，和耗散条款，如2.5PN效应，轨道硬化的外二进制，和影响的动力学摩擦的入侵者动力学的早期阶段。在这一系列的第一篇论文致力于研究从宇宙学的角度来看，MBH三胞胎的动力学，我们描述，测试和验证我们的代码。
英文摘要：
Massive black-hole binaries (MBHBs) are thought to be the main source of gravitational waves (GWs) in the low-frequency domain surveyed by ongoing and forthcoming Pulsar Timing Array campaigns and future space-borne missions, such as {\it eLISA}. However, many low-redshift MBHBs in realistic astrophysical environments may not reach separations small enough to allow significant GW emission, but rather stall on (sub)pc-scale orbits. This "last-parsec problem" can be eased by the appearance of a third massive black hole (MBH) -- the "intruder" -- whose action can force, under certain conditions, the inner MBHB on a very eccentric orbit, hence allowing intense GW emission eventually leading to coalescence. A detailed assessment of the process, ultimately driven by the induced Kozai-Lidov oscillations of the MBHB orbit, requires a general relativistic treatment and the inclusion of external factors, such as the Newtonian precession of the intruder orbit in the galactic potential and its hardening by scattering off background stars. In order to tackle this problem, we developed a three-body Post-Newtonian (PN) code framed in a realistic galactic potential, including both non-dissipative 1PN and 2PN terms, and dissipative terms such as 2.5PN effects, orbital hardening of the outer binary, and the effect of the dynamical friction on the early stages of the intruder dynamics. In this first paper of a series devoted at studing the dynamics of MBH triplets from a cosmological perspective, we describe, test and validate our code.
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