Abstract We have constructed self-similar models of a time-dependent accretion disk in both sub and super-Eddington phases with wind outflows for tidal disruption events (TDEs). The physical input parameters are the black hole (BH) mass M•, specific orbital energy E and angular momentum J, star mass M⋆ and radius R⋆. We consider the sub-Eddington phase to be total pressure (model A1) and gas pressure (model A2) dominated. In contrast, the super-Eddington phase is dominated by radiation pressure (model B) with Thomson opacity. We derive the viscosity prescribed by the stress tensor, Π r ϕ ∝ Σ d b r d where Σd is the surface density of the disk, r is the radius and b and d are constants. The specific choice of radiative or α viscosity is motivated, and its parameters are decided by the expected disk luminosity and evolution time scale being in the observed range. The disk evolves due to mass loss by accretion onto the black hole and outflowing wind, and mass gain by fallback of the debris; this results in an increasing outer radius. We have simulated the luminosity profile for both sub and super-Eddington disks. As an illustrative example, we fit our models to the observations in X-ray, UV, and Optical of four TDE events and deduce the physical parameters above.

中文翻译：

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潮汐破坏事件中的吸积和风动力学

摘要 我们已经构建了具有潮汐干扰事件 (TDE) 风外流的亚爱丁顿相和超爱丁顿相的时间相关吸积盘的自相似模型。物理输入参数是黑洞 (BH) 质量 M•、比轨道能量 E 和角动量 J、恒星质量 M⋆ 和半径 R⋆。我们认为亚爱丁顿相以总压力（模型 A1）和气体压力（模型 A2）为主。相比之下，超爱丁顿相由具有汤姆森不透明度的辐射压力（模型 B）主导。我们推导出由应力张量 Π r ϕ ∝ Σ dbrd 规定的粘度，其中 Σd 是圆盘的表面密度，r 是半径，b 和 d 是常数。辐射或α粘度的具体选择是有动机的，其参数由观测范围内的预期圆盘光度和演化时间尺度决定。由于吸积到黑洞和外流风导致质量损失，以及碎片回落导致质量增加，圆盘演化；这导致外半径增加。我们模拟了亚爱丁顿圆盘和超爱丁顿圆盘的光度分布。作为说明性示例，我们将我们的模型与四个 TDE 事件的 X 射线、UV 和光学观测值相匹配，并推导出上述物理参数。