原行星盘的内缘结构
The Inner Rim Structures of Protoplanetary Discs
摘要：
原行星盘的内边界由含尘区向无尘区过渡时不透明度的剧烈变化构成。本文探讨了被动加热含尘圆盘内边缘结构的变化及其局限性。在这项研究中，我们实现了详细的升华物理快速蒙特卡罗辐射转移代码。结果表明，尘埃盘的内缘不是一个无限尖锐的壁，而是一个可宽可窄的扩散区。此外，高表面密度和大的硅酸盐颗粒，以及铁和铁的颗粒会降低边缘半径，从47太阳光度的赫比格Ae恒星周围的小硅酸盐的2.2天文单位半径通常到0.4天文单位和接近0.2天文单位。因此，具有晶粒生长和不同粉尘成分的被动盘必须具有小的内边缘半径。最后，给出了边缘位置随尘埃、星盘和恒星性质变化的解析表达式。
英文摘要：
The inner boundary of protoplanetary discs is structured by the dramatic opacity changes at the transition from the dust-containing to a dust-free zone. This paper explores the variety and limits of inner rim structures in passively heated dusty discs. For this study, we implemented detailed sublimation physics in a fast Monte Carlo radiative transfer code. We show that the inner rim in dusty discs is not an infinitely sharp wall but a diffuse region which may be narrow or wide. Furthermore, high surface densities and large silicate grains as well as iron and corundum grains decrease the rim radius, from a 2.2AU radius for small silicates around a 47 Solar luminosity Herbig Ae star typically to 0.4AU and as close as 0.2AU. A passive disc with grain growth and a diverse dust composition must thus have a small inner rim radius. Finally, an analytical expression is presented for the rim location as a function of dust, disc and stellar properties.
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