论文标题
冷却对围环盘的积聚的影响，使超大的黑洞二进制
The effect of cooling on the accretion of circumprimary discs inmerging supermassive black hole binaries
论文作者
论文摘要
在超大黑洞结合的最后阶段，重力波的发射将有效地从二进制轨道上消除能量和角动量，从而使紧凑物体之间的分离缩小。在存在环绕盘的情况下，将会发展出挤压阶段，其中圆盘与次级黑洞之间的潮汐相互作用可以将气体向内推动，从而提高了对主要的积聚率并产生所谓的电磁前体。在这种情况下，使用3D流体动力模拟，我们研究了绝热围环积光盘如何响应随着次要落在更大的物体上的变化重力潜力。我们包括了由参数β=ωt_{cool}控制的冷却处方，该处方将确定最终吸积率的强度：更热的光盘较厚，并且潮汐相互作用被抑制了二进制平面外的气体。我们的主要结果是，对于气体无法快速冷却（β> 30）的场景（β> 30），盘变得厚并使系统看不见，而对于β<10，强烈的冷却阻止了次级轨道上的任何泄漏，从而使增强速度的增强速率提高了两个数量级，则在模拟的其余部分中，强度强于平均值。
At the final stages of a supermassive black hole coalescence, the emission of gravitational waves will efficiently remove energy and angular momentum from the binary orbit, allowing the separation between the compact objects to shrink. In the scenario where a circumprimary disc is present, a squeezing phase will develop, in which the tidal interaction between the disc and the secondary black hole could push the gas inwards, enhancing the accretion rate on to the primary and producing what is known as an electromagnetic precursor. In this context, using 3D hydrodynamic simulations, we study how an adiabatic circumprimary accretion disc responds to the varying gravitational potential as the secondary falls onto the more massive object. We included a cooling prescription controlled by the parameter β= Ωt_{cool}, which will determine how strong the final accretion rate is: a hotter disc is thicker, and the tidal interaction is suppressed for the gas outside the binary plane. Our main results are that for scenarios where the gas cannot cool fast enough (β>30) the disc becomes thick and renders the system invisible, while for β<10 the strong cooling blocks any leakage on to the secondary's orbit, allowing an enhancement in the accretion rate two orders of magnitude stronger than the average through the rest of the simulation.
