论文标题
主磁盘及其在崩溃的磁旋转原恒星云中的观察磁盘外观
Primary disks and their observational appearance in collapsing magnetic rotating protostellar clouds
论文作者
论文摘要
磁旋转原恒星云的崩溃，质量为$ 10 \，m _ {\ odot} $的崩溃是数值研究的。云的热，磁性和旋转能量与其重力能量的模量的初始比分别为0.3、0.2和0.01。重点是在崩溃的等温阶段形成的准磁静脉主要盘的演化和特性。仿真表明，从$ 1500 $ au和$ 7400 $ au和$ 0.3 \，m _ {\ odot} $增长到$ 5.2 \，M _ {\ odot} $，主磁盘的大小和质量增加。磁场是云包膜中的准radial，主要磁盘中的准均匀均匀。快速冲击MHD波的前面产生环形磁场，该波从初级磁盘边界和在第一个静水压芯附近形成的流出区域中传播。在磁场的几何形状和角动量分布方面，可以在观测中揭示塌陷的原始云的分层结构。
The collapse of the magnetic rotating protostellar cloud with mass of $10\,M_{\odot}$ is numerically studied. The initial ratios of the thermal, magnetic, and rotational energies of the cloud to the modulus of its gravitational energy are 0.3, 0.2 and 0.01, respectively. The emphasis is on the evolution and properties of the quasi-magnetostatic primary disk formed at the isothermal stage of the collapse. Simulations show that the primary disk size and mass increase during evolution from $1500$ au to $7400$ au and from $0.3\,M_{\odot}$ to $5.2\,M_{\odot}$, respectively. Magnetic field is quasi-radial in the cloud envelope and quasi-uniform within the primary disk. A toroidal magnetic field is generated behind the front of the fast shock MHD wave propagating from the primary disk boundary and in the region of the outflow formed near the first hydrostatic core. The hierarchical structure of collapsing protostellar clouds can be revealed in observations in terms of the magnetic field geometry and the angular momentum distribution.
