FAST COALESCENCE OF MASSIVE BLACK HOLE BINARIES FROM MERGERS OF GALACTIC NUCLEI: IMPLICATIONS FOR LOW-FREQUENCY GRAVITATIONAL-WAVE ASTROPHYSICS
FAST COALESCENCE OF MASSIVE BLACK HOLE BINARIES FROM MERGERS OF GALACTIC NUCLEI: IMPLICATIONS FOR LOW-FREQUENCY GRAVITATIONAL-WAVE ASTROPHYSICS
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DOI：
10.1088/2041-8205/732/2/l26
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发表时间：
2011-02
期刊：
影响因子：
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通讯作者：
M. Preto;I. Berentzen;P. Berczik;R. Spurzem
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作者：
M. Preto;I. Berentzen;P. Berczik;R. Spurzem
我们研究了最终秒差距问题的纯恒星动力学解决方案。主要合并产生的星系核不是球形的，而是表现出一定程度的三轴性。通过 N 体模拟，我们表明，它们所承载的等质量大质量黑洞双星 (MBHB) 将持续与亲心轨道上的恒星相互作用，从而在比哈勃时间短得多的时间内吸气，直至分离，此时引力波 (GW) 发射的强度足以驱动它们合并。这种聚结将成为未来星载探测器（例如激光干涉仪空间天线（LISA））的重要引力波来源。根据我们对等质量并合的结果，并考虑到不等质量双星的硬化率相似，我们预计 LISA 每年将看到约 10 到约几个 × 102 的此类事件，具体取决于最近对星系并合树和 MBH 协同演化的研究中获得的特定大质量黑洞 (MBH) 种子模型。当 e ≳ 0.001–0.01 时，LISA 带中的轨道偏心率将明显不同于零。
We investigate a purely stellar dynamical solution to the Final Parsec Problem. Galactic nuclei resulting from major mergers are not spherical, but show some degree of triaxiality. With N-body simulations, we show that equal-mass massive black hole binaries (MBHBs) hosted by them will continuously interact with stars on centrophilic orbits and will thus inspiral—in much less than a Hubble time—down to separations at which gravitational-wave (GW) emission is strong enough to drive them to coalescence. Such coalescences will be important sources of GWs for future space-borne detectors such as the Laser Interferometer Space Antenna (LISA). Based on our results for equal-mass mergers, and given that the hardening rate of unequal-mass binaries is similar, we expect that LISA will see between ∼10 and ∼ few × 102 such events every year, depending on the particular massive black hole (MBH) seed model as obtained in recent studies of merger trees of galaxy and MBH co-evolution. Orbital eccentricities in the LISA band will be clearly distinguishable from zero with e ≳ 0.001–0.01.