盘占优势阶段潮汐破坏事件的统一模型
A unified model of tidal destruction events in the disc-dominated phase
摘要：
我们开发了一个统一的计划，解释了不同的观察到的性质的TDEs在简单的磁盘物理。统一计划假设，不同的观测到的TDEs的属性控制的峰值爱丁顿比的吸积盘形成后，恒星分裂。我们的主要结果是，TDE人口可以分为四个亚群，这是（按峰值爱丁顿比下降的顺序）：“模糊”的UV明亮和X射线暗淡的TDE; X射线明亮的软态TDE; UV明亮和X射线暗淡的“冷”TDE;和X射线明亮的硬态TDE。这4个TDE子群将发生在质量定义明确的黑洞周围，因此我们的统一方案可以直接用观测来检验。作为初始测试，我们对取自四个亚群中的三个的六个TDE的X射线和UV光曲线进行建模：ASASSN-14 ae、ASASSN-15 oi、ASASSN-18 pg、AT 2019 dsg、XMMSL 1 J 0740和XMMSL 2 J1446。我们发现，所有六个TDE，跨越了广泛的观察到的属性，以及不断发展的相对论薄盘建模。六个最佳拟合圆盘解的峰值爱丁顿比与统一模型的预测完全一致。六个源的平均恒星质量是$\left\langle M_\star \right\rangle \sim 0.24 M_\odot$。所谓的“失踪的能量问题”的解决，证明只有$\sim 1\%$的辐射吸积盘能量在X射线和紫外线频率观察。最后，我们提出了一个经验，近似线性，吸积盘的总辐射能量和总辐射能量的早期，快速衰减，紫外线组件，在所有的TDEs之间的关系。
英文摘要：
We develop a unification scheme which explains the varied observed properties of TDEs in terms of simple disc physics. The unification scheme postulates that the different observed properties of TDEs are controlled by the peak Eddington ratio of the accretion discs which form following a stellar disruption. Our primary result is that the TDE population can be split into four subpopulations, which are (in order of decreasing peak Eddington ratio): "obscured" UV-bright and X-ray dim TDEs; X-ray bright soft-state TDEs; UV-bright and X-ray dim "cool" TDEs; and X-ray bright hard-state TDEs. These 4 subpopulations of TDEs will occur around black holes of well defined masses, and our unification scheme is therefore directly testable with observations. As an initial test, we model the X-ray and UV light curves of six TDEs taken from three of the four subpopulations: ASASSN-14ae, ASASSN-15oi, ASASSN-18pg, AT2019dsg, XMMSL1 J0740 & XMMSL2 J1446. We show that all six TDEs, spanning a wide range of observed properties, are well modelled by evolving relativistic thin discs. The peak Eddington ratio's of the six best-fitting disc solutions lie exactly as predicted by the unified model. The mean stellar mass of the six sources is $\left\langle M_\star \right\rangle \sim 0.24 M_\odot$. The so-called `missing energy problem' is resolved by demonstrating that only $\sim 1\%$ of the radiated accretion disc energy is observed at X-ray and UV frequencies. Finally, we present an empirical, approximately linear, relationship between the total radiated energy of the accretion disc and the total radiated energy of an early-time, rapidly-decaying, UV component, seen in all TDEs.
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