论文标题
潮汐破坏事件中的积聚和风的动力学
Dynamics of accretion and winds in tidal disruption events
论文作者
论文摘要
我们已经在子和超级 - 埃德丁顿阶段的时间相关积聚磁盘上构建了自相似的模型，并具有潮汐破坏事件（TDES）的风流。物理输入参数是黑洞（BH）质量$ M _ {\ bullet} $，特定的轨道能$ e $和Angular Mommentum $ J $，Star Mass $ M _ {\ Star} $和RADIUS $ R _ {\ star} $。我们认为亚埃丁顿阶段是总压力（A1型）和气压（A2型）。相比之下，超级埃德丁顿阶段以汤姆森不透明的辐射压力（B）为主。我们得出应力张量规定的粘度，$π_{r ϕ} \ proptoσ_d^b r^d $其中$σ_d$是磁盘的表面密度，$ r $是半径，$ b $，$ b $，$ d $是常数。辐射或$α$粘度的特定选择是动机的，其参数由预期的磁盘光度和进化时间尺度决定在观察到的范围内决定。磁盘由于积聚到黑洞和散发风的质量损失而发展，碎屑的后备质量增加。这会导致外半径增加。我们已经模拟了子和超级 - 埃德丁顿磁盘的光度曲线。作为一个说明性的示例，我们将模型适合于X射线，UV和四个TDE事件的光学观测值，并推断上述物理参数。
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 $M_{\bullet}$, specific orbital energy $E$ and angular momentum $J$, star mass $M_{\star}$ and radius $R_{\star}$. 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, $Π_{rϕ}\propto Σ_d^b r^d$ where $Σ_d$ 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.
