磁化星际分子云 - III. 纤维碰撞与核形成：对子结构和演化的洞察
Magnetized interstellar molecular clouds - III. Filament Collisions and Core Formation: Insights into Substructures and Evolution
- Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）
- University of California at Berkeley（加州大学伯克利分校）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
通过理想磁流体动力学模拟，研究分子云中丝状结构形成与碎裂，发现亚临界子纤维碰撞合并是前恒星核形成的关键机制，并可能影响双星形成。
AI中文摘要：
我们展示了一个驱动型理想磁流体动力学分子云模拟的结果，以研究分子云中丝状结构的形成及其碎裂为致密云核的过程。激波压缩导致亚秒差距尺度的丝状结构形成。大尺度超音速流将这些小纤维推挤在一起，形成巨大的丝状云。形成的主纤维横跨模拟的整个4.4秒差距长度，其半峰全宽中位数为0.075秒差距，与在许多分子云中观测到的相似。主纤维内部的子纤维的半峰全宽中位数为0.03-0.04秒差距，类似于分子谱线中观测到的“纤维”。亚临界子纤维的碰撞与合并是前恒星核形成的重要机制。碰撞的子纤维及其交汇处产生的核构成一个枢纽-纤维系统，类似于与大质量恒星形成相关的系统，但尺度较小。核合并对前恒星核的生长可能具有重要意义，并可能在双星的形成中发挥作用。
英文摘要：
We present the results of a driven, ideal magnetohydrodynamics simulation of a molecular cloud to study the formation of filamentary structures in molecular clouds and their fragmentation into dense cloud cores. Shock compression results in the formation of sub-parsec long filamentary structures. Large-scale supersonic flows push these small filaments together and form massive filamentary clouds. The main filament that forms stretches across the full 4.4 pc length of the simulation and has a median FWHM of 0.075 pc, similar to that observed in many molecular clouds. Subfilaments inside the main filament have a median FWHM of 0.03-0.04 pc, similar to the ``fibers" observed in molecular lines. The collision and merger of subcritical subfilaments is an important mechanism for the formation of prestellar cores. Colliding subfilaments and the resulting core at their intersection is a hub-filament system similar to that associated with massive star formation, but on a smaller scale. Core mergers can be significant in the growth of pre-stellar cores and may play a role in the formation of binary stars.
