论文标题
相互作用的Kilonovae：与活性银河核的积聚磁盘中的二进制合并的持久电磁对应物
Interacting Kilonovae: Long-lasting Electromagnetic Counterparts to Binary Mergers in the Accretion Disks of Active Galactic Nuclei
论文作者
论文摘要
我们研究了在活性银河核（AGN）的增生盘中发生的中子星形中子星（NS-NS）或中子星形黑色孔（NS-BH）合并弹出的动力学和电磁（EM）特征。我们发现，射流和磁盘气体之间的相互作用会对动力学和辐射产生重要影响。我们展示了射流动力学的五个阶段：重力放慢，沿海，磁盘中的塞多夫·泰勒减速，从磁盘表面突破后的重新加速以及势头保存的雪带阶段。同时，从射出的辐射非常明亮，以至于其典型的峰光度达到几次$ 10^{43} -10^{44}〜\ rm erg erg〜s^{ - 1} $。由于大多数辐射能已经从合并弹射的动能转化，因此我们称这种爆炸性现象为相互作用的Kilonova（IKN）。应该强调的是，ikne与AGN磁盘中NS-NS/BH-NS合并事件非常有前途，明亮的EM对应物。明亮的峰值光度和较长的上升时间（即紫外线带10到二十天，光带中的三十至五十天，在IR频段中为一百天到数百天）使大多数调查望远镜都有足够的时间来检测IKN。然而，IKN的光曲线的峰亮度，峰值时间和演变模式类似于银河核中的超浮肿超新星和潮汐破坏事件，因此很难区分它们。但这也表明ikne可能存在于记录的AGN瞬变中。
We investigate the dynamics and electromagnetic (EM) signatures of neutron star-neutron star (NS-NS) or neutron star-black hole (NS-BH) merger ejecta that occurs in the accretion disk of an active galactic nucleus (AGN). We find that the interaction between ejecta and disk gas leads to important effects on the dynamics and radiation. We show five stages of the ejecta dynamics: gravitational slowing down, coasting, Sedov-Taylor deceleration in the disk, re-acceleration after the breakout from the disk surface, and momentum-conserved snowplow phase. Meanwhile, the radiation from the ejecta is so bright that its typical peak luminosity reaches a few times $10^{43}-10^{44}~\rm erg~s^{-1}$. Since most of the radiation energy has converted from the kinetic energy of merger ejecta, we call such an explosive phenomenon an interacting kilonova (IKN). It should be emphasized that IKNe are very promising, bright EM counterparts to NS-NS/BH-NS merger events in AGN disks. The bright peak luminosity and long rising time (i.e., ten to twenty days in UV bands, thirty to fifty days in optical bands, and one hundred days to hundreds of days in IR bands) allow most survey telescopes to have ample time to detect an IKN. However, the peak brightness, peak time, and evolution pattern of the light curve of an IKN are similar to a superluminous supernova in a galactic nucleus and a tidal disruption event making it difficult to distinguish between them. But it also suggests that IKNe might have been present in recorded AGN transients.
