Coalescing binary black holes experience a "kick" due to anisotropic emission of gravitational waves with an amplitude as great as ～200 km s~(-1). We examine the orbital evolution of black holes that have been kicked from the centers of triaxial galaxies. Timescales for orbital decay are generally longer in triaxial galaxies than in equivalent spherical galaxies, since a kicked black hole does not return directly through the dense center where the dynamical friction force is highest. We evaluate this effect by constructing self-consistent triaxial models and integrating the trajectories of massive particles after they are ejected from the center; the dynamical friction force is computed directly from the velocity dispersion tensor of the self-consistent model. We find return times that are several times longer than in a spherical galaxy with the same radial density profile, particularly in galaxy models with dense centers, implying a substantially greater probability of finding an off-center black hole.
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机译：由于各向异性发射出的重力波振幅高达〜200 km s〜（-1），聚结的二元黑洞会经历“拐点”。我们研究了从三轴星系中心踢出的黑洞的轨道演变。在三轴星系中，轨道衰减的时间尺度通常比在等效球形星系中更长，因为有脚踢的黑洞不会直接通过动摩擦力最高的密集中心返回。我们通过构建自洽的三轴模型并整合从中心弹出的大颗粒的轨迹来评估这种效果。动摩擦力直接从自洽模型的速度弥散张量中计算得出。我们发现返回时间比具有相同径向密度分布的球形星系要长几倍，特别是在具有密集中心的星系模型中，这意味着发现偏心黑洞的可能性要大得多。
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