论文标题
AGN中的辐射性，对流尘埃磁盘的物理模型
A physical model for radiative, convective dusty disk in AGN
论文作者
论文摘要
主动银河核（AGN）中的吸积盘藏有外部照明的灰尘：在圆盘的中间平面左右，大约$ m _ {\ rm bh} = 10^{7} {7} m _ {\ odot} $黑洞，灰尘可以在0.1美元的$ 0.1 $ pc上与0.5pc相比。我们构建了一个圆盘区域的物理模型，该模型大约位于磁盘中平面的灰尘升华半径与圆盘表面灰尘升华的半径之间。我们的主要结论是，对于广泛的模型参数，例如局部积聚率和/或不透明度，积聚磁盘自身对灰尘的辐射压力显着影响其垂直结构。除了高度对流之外，这种磁盘还可以从几何变细到纤细。我们的模型适合Czerny＆Hryniewicz（2011）和Baskin＆Laor（2018）的“紧凑型Torus”模型的“失败风”场景的叙述，并将它们作为辐射性尘埃磁盘模型的变化结合在一起。
An accretion disk in an Active Galactic Nucleus (AGN) harbors and shields dust from external illumination: at the mid-plane of the disk around a $M_{\rm BH}=10^{7}M_{\odot}$ black hole, dust can exist at $0.1$pc from the black hole, compared to 0.5pc outside of the disk. We construct a physical model of a disk region approximately located between the radius of dust sublimation at the disk mid-plane and the radius at which dust sublimes at the disk surface. Our main conclusion is that for a wide range of model parameters such as local accretion rate and/or opacity, the accretion disk's own radiation pressure on dust significantly influences its vertical structure. In addition to being highly convective, such a disk can transform from geometrically thin to slim. Our model fits into the narrative of a "failed wind" scenario of Czerny & Hryniewicz (2011) and the "compact torus" model of Baskin & Laor (2018), incorporating them as variations of the radiative dusty disk model.
