论文标题
角臂，磁化和原始核心的积聚
Angular Momenta, Magnetization, and Accretion of Protostellar Cores
论文作者
论文摘要
基于我们先前对恒星形成分子气体在以前的工作中重力塌陷中形成的云核的角动力学研究的基础，我们现在检查核心特性，假设理想的磁性水力动力学（MHD）。使用相同的接收点实现，我们对\ emph {athena} MHD代码进行了表征，我们表征了核心的统计特性，包括质量积聚率，特定的角动量以及磁场和核心旋转轴之间的对齐$ 0.1 \ \ \ \ \ \ \ \ \ \ \ \ m mathrm {pc} $比例。我们的模拟重现了观察到的磁场强度和气体密度之间的关系，它表明磁场可以帮助对低密度流程进行对线，并帮助种子丝状结构的位置。与我们以前的纯流体动力学模拟一致，在细丝的异质环境中形成恒星（接收器），使得在核心上吸收具有高度的发作性，导致短期变异性，但没有特定角度臂的长期单调生长。通过统计特征的原始核心特性和行为，我们旨在为建立更现实和自洽的磁盘形成模型提供一个起点，从而有助于解决磁场是否可以防止理想MHD限制中（大的）偶然磁盘的发展。
Building on our previous hydrodynamic study of the angular momenta of cloud cores formed during gravitational collapse of star-forming molecular gas in our previous work, we now examine core properties assuming ideal magnetohydrodynamics (MHD). Using the same sink-patch implementation for the \emph{Athena} MHD code, we characterize the statistical properties of cores, including the mass accretion rates, specific angular momenta, and alignments between the magnetic field and the spin axis of the core on the $0.1 \ \mathrm{pc}$ scale. Our simulations, which reproduce the observed relation between magnetic field strength and gas density, show that magnetic fields can help collimate low density flows and help seed the locations of filamentary structures. Consistent with our previous purely hydrodynamic simulations, stars (sinks) form within the heterogeneous environments of filaments, such that accretion onto cores is highly episodic leading to short-term variability but no long-term monotonic growth of the specific angular momenta. With statistical characterization of protostellar cores properties and behaviors, we aim to provide a starting point for building more realistic and self-consistent disk formation models, helping to address whether magnetic fields can prevent the development of (large) circumstellar disks in the ideal MHD limit.
