论文标题
猎户座B中的旋转细丝：核心是否从父丝中继承了它们的角动量？
Rotating filament in Orion B: Do cores inherit their angular momentum from their parent filament?
论文作者
论文摘要
角动量是控制恒星形成的最重要的物理量之一。核心的初始角动量可能导致其碎片化，并可能影响原球盘的大小。为了了解核心如何获得其初始角动量，重要的是研究它们形成的细丝的角动量。尽管已经探索了有关细丝旋转的理论研究，但在恒星形成细丝中，特定角动量的观察测量很少。我们介绍了Orion B中LBS 23（HH24-HH26）区域的高分辨率N2D+ ALMA观测值，该区域在星形灯丝中提供了特定角动量最可靠的测量之一。我们找到了总特定的角动量（$ 4 \ times 10^{20} cm^2s^{ - 1} $），特定的角动量与半径（j（r）$ \ propto r^{1.83} $）的依赖性，以及旋转能量的比例，腐烂的比例（$β_腐烂）的比例（$β{$β{$β{$β{在其他星形区域中，我们的细丝宽度（$ \ sim $ 0.04 PC）。我们的细丝角动量轮廓与从环境湍流中获得的旋转以及显示核心及其宿主丝同时发展的模拟一致，这是由于湍流产生的非线性扰动的多尺度生长。
Angular momentum is one of the most important physical quantities that govern star formation. The initial angular momentum of a core may be responsible for its fragmentation and can have an influence on the size of the protoplanetary disk. To understand how cores obtain their initial angular momentum, it is important to study the angular momentum of filaments where they form. While theoretical studies on filament rotation have been explored, there exist very few observational measurements of the specific angular momentum in star-forming filaments. We present high-resolution N2D+ ALMA observations of the LBS 23 (HH24-HH26) region in Orion B, which provide one of the most reliable measurements of the specific angular momentum in a star-forming filament. We find the total specific angular momentum ($4 \times 10^{20} cm^2s^{-1}$), the dependence of the specific angular momentum with radius (j(r) $\propto r^{1.83}$), and the ratio of rotational energy to gravitational energy ($β_{rot} \sim 0.04$) comparable to those observed in rotating cores with sizes similar to our filament width ($\sim$ 0.04 pc) in other star-forming regions. Our filament angular momentum profile is consistent with rotation acquired from ambient turbulence and with simulations that show cores and their host filaments develop simultaneously due to the multi-scale growth of nonlinear perturbation generated by turbulence.
