论文标题
部分可观测时空混沌系统的无模型预测
Final stage of merging binaries of supermassive black holes: observational signatures
论文作者
论文摘要
对二元超质量黑洞（SMBH）的兴趣越来越大，但是将二进制组合成小于〜1光天（〜10^2的重力半径为10^8 msun），在重力控制下迅速演变，在观察结果中是难以捉摸的。在本文中，我们讨论了三个制度的组件SMBH周围小盘的命运：1）低率（以对流为主的积聚流量：ADAFS）； 2）中级费率； 3）超级 - 埃德丁顿积聚率。具有中间速率的迷你盘正在通过形成混合径向结构的热电晕传导通过热传导。当二进制轨道时期短于蒸发迷你盘的声音传播时间尺度时，出现了一种新的不稳定，称为声音不稳定性，因为磁盘会高度扭曲，以使它们被破坏。我们证明了与迷你盘的声音不稳定性的A_ {Crit} 〜10^2 rg的临界分离，并且腔体充满了热气体。对于这些二进制文件，组件SMBHS在ADAF制度中以Bondi模式积聚，显示出由于轨道运动引起的ADAF的多普勒增强效应而产生的周期性变化。同时，环形磁盘（CBD）仍然不够热（紫外线缺陷），无法产生光子以使气体对宽发射线的电离电离。对于CBD的略微超级 - 埃德丁顿积聚，MGII线出现紫外线赤字的减少，对于中级超级 - 埃德丁顿Balmer线，除非CIV线，否则除非CBD积聚率非常高，否则CIV线永远不会。此外，如果CBD与二元平面未对准，则预计它具有光学周期性变化，而无线电周期约十倍。
There are increasing interests in binary supermassive black holes (SMBHs), but merging binaries with separations smaller than ~1 light days (~10^2 gravitational radii for 10^8 Msun), which are rapidly evolving under control of gravitational waves, are elusive in observations. In this paper, we discuss fates of mini-disks around component SMBHs for three regimes: 1) low rates (advection-dominated accretion flows: ADAFs); 2) intermediate rates; 3) super-Eddington accretion rates. Mini-disks with intermediate rates are undergoing evaporation through thermal conduction of hot corona forming a hybrid radial structure. When the binary orbital periods are shorter than sound propagation timescales of the evaporated mini-disks, a new instability, denoted as sound instability, arises because the disks will be highly twisted so that they are destroyed. We demonstrate a critical separation of A_{crit}~10^2 Rg from the sound instability of the mini-disks and the cavity is full of hot gas. For those binaries, component SMBHs are accreting with Bondi mode in the ADAF regime, showing periodic variations resulting from Doppler boosting effects in radio from the ADAFs due to orbital motion. In the mean while, the circumbinary disks (CBDs) are still not hot enough (ultraviolet deficit) to generate photons to ionize gas for broad emission lines. For slightly super-Eddington accretion of the CBDs, MgII line appears with decreases of UV deficit, and for intermediate super-Eddington Balmer lines appear, but CIV line never unless CBD accretion rates are extremely high. Moreover, if the CBDs are misaligned with the binary plane, it is then expected to have optical periodical variations with about ten times radio periods.
