Star formation in turbulent cloud cores with magnetic diffusion

分子云核心经历引力坍缩形成原恒星和原行星盘。观测表明，分子云核心具有磁场和湍流。磁场具有耗散机制，特别是在高密度气体中。在本研究中，我们研究了考虑磁耗散的磁化和湍流分子云核的坍缩。通过高分辨率自适应网格细化（AMR）模拟，我们跟踪了云核从坍缩开始到形成原恒星和原行星盘的演化过程。所有的云核都会产生原行星盘，而不考虑磁场和湍流的假设强度。有一种趋势是，强磁场模型显示原行星盘的生长速度较慢。强磁场模型在落包络层中表现出空腔，这是由磁场的交换不稳定性引起的。

A molecular cloud core undergoes gravitational collapse to form a protostar and protoplanetary disk. Observations suggest that molecular cloud cores have magnetic field and turbulence. The magnetic field has a dissipative mechanism especially in the high-density gas.In this study, we investigated collapse of magnetized and turbulent molecular cloud cores, taking account of magnetic dissipation. We fallowed the evolution of the cloud cores from onset of collapse to formation of a protostar and protoplanetary disk, by using high-resolution adaptive mesh refinement (AMR) simulations. All the cloud cores produce protoplanetary disks irrespective of assumed strengths of magnetic field and turbulence. There is a tendency that a strong magnetic field model shows slower growth of a protoplanetary disk. The strong magnetic field models exhibit cavities in the infalling envelopes, which are caused by the interchange instability of the magnetic field.