低质量恒星形成的驱动和衰减Turbulence模拟：从团块到核心再到原恒星
Driven and Decaying Turbulence Simulations of Low-Mass Star Formation: From Clumps to Cores to Protostars
摘要：
分子云被观察到是湍流的，但这种湍流的起源还没有很好的理解。因此，有两种不同的方法来模拟分子云，一种是在初始化后允许湍流衰减，另一种是驱动湍流。我们使用的自适应网格细化（AMR）代码，猎户座，进行高分辨率的模拟分子云核心和原恒星的环境驱动和衰减湍流。我们包括自重力，使用正压状态方程，并表示区域超过最大网格分辨率与汇粒子。我们分析了束缚核的性质，如大小，形状，线宽和转动能，我们发现与观测合理的协议。在高分辨率下，两种情况下不同的核吸积速率对原恒星系统的发展有着重要的影响。在一个衰减的湍流环境中形成的团块产生高多重性的原恒星系统与Toomre-Q不稳定盘，表现出竞争性吸积模型的恒星形成的特点。相比之下，核心形成的背景下，不断驱动的湍流和维里平衡形式较小的原恒星系统，具有较少的低质量的成员。我们对驱动和衰减湍流的模拟显示出一些统计上的显著差异，特别是在褐矮星和核心旋转的产生方面，但不确定性足够大，我们无法得出结论，观察结果是否有利于其中一个。
英文摘要：
Molecular clouds are observed to be turbulent, but the origin of this turbulence is not well understood. As a result, there are two different approaches to simulating molecular clouds, one in which the turbulence is allowed to decay after it is initialized, and one in which it is driven. We use the adaptive mesh refinement (AMR) code, Orion, to perform high-resolution simulations of molecular cloud cores and protostars in environments with both driven and decaying turbulence. We include self-gravity, use a barotropic equation of state, and represent regions exceeding the maximum grid resolution with sink particles. We analyze the properties of bound cores such as size, shape, linewidth, and rotational energy, and we find reasonable agreement with observation. At high resolution, the different rates of core accretion in the two cases have a significant effect on protostellar system development. Clumps forming in a decaying turbulence environment produce high-multiplicity protostellar systems with Toomre-Q unstable disks that exhibit characteristics of the competitive accretion model for star formation. In contrast, cores forming in the context of continuously driven turbulence and virial equilibrium form smaller protostellar systems with fewer low-mass members. Our simulations of driven and decaying turbulence show some statistically significant differences, particularly in the production of brown dwarfs and core rotation, but the uncertainties are large enough that we are not able to conclude whether observations favor one or the other.
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