Binary Formation in Turbulent Magnetized Molecular Cloud Cores

这项工作的目的是了解如何在湍流分子云核中形成恒星，特别是双星。由于双星是由于分子云核的引力崩塌而形成的，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，我们研究了母体湍流分子云形成分子云核的过程。恒星形成的分子云是湍流和磁化的。因此，我们使用三维磁流体力学程序来探索分子云的形成。我们的模拟表明，分子云核是由湍流分子云通过湍流压缩形成的。由于外界的湍流压力，如此形成的云核往往具有拉长的形状。此外，由于湍流运动导致的剪切运动仍留在岩心中。这种剪切运动对于在这样的云核中形成双星非常重要。这种核碎裂的条件k可由旋转能与引力能之比和伸长度给出。由湍流云形成的核心通常有足够的k个核心碎裂的自转。因此，双星很可能很容易由湍急的分子云形成。在岩心形成过程中，外部湍流压力起着重要作用，有时甚至超过自重。

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.