Binary Formation in Turbulent Magnetized Molecular Cloud Cores

这项工作的目的是了解如何形成恒星，特别是在湍流分子云核心的双星。由于双星是由分子云核的引力坍缩而形成的，因此弄清母体分子云核的物理性质是非常重要的。在这项研究中，我们fug研究了分子云核心的形成过程，从母体湍流分子云。形成星星的分子云是动荡的和磁化的。因此，我们使用三维磁流体动力学代码来探索分子云的形成。我们的模拟结果表明，分子云的核心是通过湍流压缩从湍流分子云。这样形成的云核由于外部湍流压力的作用而趋于拉长的形状。此外，由于湍流运动的剪切运动仍然在核心。这种切变运动对于在这种云核中形成双星是很重要的。这类核的破碎条件k可以由自转能与引力能的比值和伸长度给出。由湍流云形成的核心通常具有足够k核心碎片的旋转。因此，双星很可能很容易从湍流分子云中形成。在核的形成过程中，外部湍流压力起着重要的作用，有时甚至超过自重力。

The purpose of this work is to understand how to form stars, in particular binary stars in turbulent molecular cloud cores. Since binary stars from due to gravitational collapse of molecular cloud cores, it is very important to clarify the physical properties of parent molecular cloud cores. In this study, we fug investigated the formation process of molecular cloud cores from parent turbulent molecular clouds. Star forming molecular clouds are turbulent and magnetized. Thus, we use a three-dimensional magneto-hydrodynamical code to explore the formation of molecular clouds. Our simulations show that molecular cloud cores are formed via turbulent compression from turbulent molecular clouds. The cloud cores so formed tend to have elongated shapes because of external turbulent pressures. Furthermore, shear motions due to turbulent motions remain in the cores. Such shear motions are important for formation of binary stars in such cloud cores. The condition k fragmentation of such cores can be given by the ratio of rotation energy to the gravitational energy and the degree of elongation. The cores formed out of turbulent clouds typically have rotation that is enough k core fragmentation. Thus, binary stars are likely to form very easily from turbulent molecular clouds. In the course of core formation, external turbulent pressures play an important role, and sometimes dominate over the self-gravity.