AI 中文总结
研究类 OJ 287 超大质量黑洞双星中盘交叉相遇时的流体动力学响应，用三维光滑粒子流体动力学模拟，探究次级黑洞质量等因素对黑洞吸积质量的影响，发现扰动体质量大时主黑洞吸积率有显著峰值及相关规律，还指出次级黑洞会有吸积盘及相关特征。
AI 中文摘要
我们研究了由耀变体 OJ 287 中观测到的准周期爆发所激发的，在倾斜、偏心轨道上的低质量黑洞刺穿大质量黑洞吸积盘的流体动力学响应。使用三维光滑粒子流体动力学模拟，我们探究了次级黑洞的质量和轨道偏心率，以及盘的厚度和粘性，如何影响两个黑洞的吸积质量随时间的变化。我们发现，只有当扰动体质量相当大（$q \gtrsim 0.1$）时，盘交叉事件才会导致主黑洞吸积率出现显著峰值，且这种峰值在首次盘交叉后大约一个自由落体时间（对于 OJ 287 约为数月）后延迟出现。轨道偏心率、盘厚度和粘性会影响响应的幅度和时间结构；特别是，较高的偏心率会导致向主黑洞输送的气体量更大且延迟更小，不过$q \gtrsim 0.1$这个条件似乎是稳健的。我们还表明，当次级黑洞质量如此大时，它通常会获得一个“吸积”盘，该盘可能产生自己的发光特征。对于像 OJ 287 这样的系统，次级吸积盘可包含$10^{2 - 3} M_\odot$，如果在与轨道周期相当的时间尺度上吸积，可以通过紫外/极紫外波段热发射峰值产生接近爱丁顿次级光度。
英文摘要
We study the hydrodynamical response of a massive black hole accretion disc punctured by a lower mass black hole on an inclined, eccentric orbit, as motivated by the quasi-periodic outbursts seen in the blazar OJ 287. Using three-dimensional smoothed particle hydrodynamics simulations, we explore how the secondary black hole's mass and orbital eccentricity, and the disc thickness and viscosity, affect the time variation of mass accretion onto both black holes. We find that disc-crossing events only lead to significant spikes in the primary black hole's accretion rate when the perturber is quite massive ($q \gtrsim 0.1$) and that such spikes are delayed by roughly a free-fall time ($\sim$ months for OJ 287) after the first disc-crossing. The orbital eccentricity, disc thickness, and viscosity can influence the amplitude and temporal structure of the response; in particular, higher eccentricity causes larger and less delayed delivery of gas to the primary, however the condition $q \gtrsim 0.1$ seems to be robust. We also show that when the secondary is this massive, it generally acquires a "pickup" disc which could produce its own luminous signature. For systems like OJ 287, the secondary pickup disc can contain $10^{2-3} M_\odot$, which if accreted over a timescale comparable to the orbital period can power near-Eddington secondary luminosities with thermal emission peaking in the UV/EUV.
Comments17 pages, 5 figures
