Substructures in protoplanetary disks (PPDs), whose ubiquity was unveiled by recent Atacama Large Millimeter/submillimeter Array observations, are widely discussed regarding their possible origins. We carry out global 2D magnetohydrodynamic (MHD) simulations in axisymmetry, coupled with self-consistent ray-tracing radiative transfer, thermochemistry, and nonideal MHD diffusivities. The abundance profiles of grains are also calculated based on the global dust evolution calculation, including sintering effects. We found that dust size plays a crucial role in the ring formation around the snow lines of PPDs through the accretion process. Disk ionization structures and thus tensorial conductivities depend on the size of grains. When grains are significantly larger than polycyclic aromatic hydrocarbons (PAHs), the nonideal MHD conductivities change dramatically across each snow line of major volatiles, leading to a sudden change in the accretion process across the snow lines and the subsequent formation of gaseous rings/gaps there. Specific layout of magnetic fields can suppress wind launching in certain regions by canceling out different stress components. On the other hand, the variations of conductivities are a lot less with only PAH-sized grains in disks and then these disks retain smoother radial density profiles across snow lines.

最近的阿塔卡马大型毫米/亚毫米阵列观测揭示了原行星盘 (PPD) 中的亚结构，其无处不在的亚结构对其可能的起源进行了广泛的讨论。我们在轴对称中进行全局 2D 磁流体动力学 (MHD) 模拟，并结合自洽的射线追踪辐射传递、热化学和非理想 MHD 扩散率。颗粒的丰度剖面也基于全球尘埃演化计算，包括烧结效应。我们发现，通过吸积过程，灰尘大小在 PPD 雪线周围的环形成中起着至关重要的作用。磁盘电离结构和因此张量电导率取决于晶粒的大小。当颗粒明显大于多环芳烃 (PAH) 时，非理想的 MHD 电导率在主要挥发物的每条雪线上发生显着变化，导致雪线上的吸积过程突然发生变化，并随后在那里形成气环/气隙。磁场的特定布局可以通过抵消不同的应力分量来抑制某些区域的风发射。另一方面，由于圆盘中只有 PAH 大小的颗粒，电导率的变化要小得多，然后这些圆盘在雪线上保持更平滑的径向密度分布。