AI 中文总结
本研究通过三维磁流体动力学模拟结合合成观测，揭示80%未来大质量恒星属成团环境，其增长具间歇性，增强吸积与枢纽-纤维系统相关，强调解读相关观测需考虑投影效应。
AI 中文摘要
控制未来大质量恒星早期质量增长的过程仍知之甚少，尤其是该增长与恒星成团性及枢纽-纤维系统（Hub-filament systems, HFSs）的关联。由于位置-位置-速度（position-position-velocity, PPV）数据中的投影效应与视线方向混淆会扭曲固有纤维结构的信息，观测上难以建立这种关联。为探究该关联，我们采用恒星形成的三维磁流体动力学（magnetohydrodynamic, MHD）模拟，其中恒星由吸积汇粒子表征。我们识别了恒星成团环境，重建了随时间变化的吸积历史，并研究了增强吸积事件与HFS位置的关系；还利用线辐射转移建模生成合成分子线观测，探究相同结构在投影PPV数据中的呈现方式。模拟中发现，80%的未来大质量恒星与成团环境相关，其增长具有高度间歇性：约40%的吸积质量来自仅占总增长时间约10%的增强吸积阶段。增强吸积阶段更靠近三维HFS代理，暗示HFS形态与未来大质量恒星的间歇性吸积可能存在关联。总体而言，结果表明未来大质量恒星的早期增长与其成团环境及周围气体的HFS结构相关，解读PPV数据中的HFS时必须考虑投影效应。
英文摘要
The processes controlling the early mass growth of future massive stars remain poorly understood, particularly the connection of this growth to star clustering and hub-filament systems (HFSs). This connection is difficult to establish observationally, because projection effects and line-of-sight confusion in position-position-velocity (PPV) data can distort the information about the intrinsic filamentary structure. To investigate this connection, we used a three-dimensional magnetohydrodynamic (MHD) simulation of star formation, where stars are represented by accreting sink particles. We identify clustered stellar environments, reconstruct time-dependent accretion histories, and investigate the relation between enhanced-accretion episodes and the locations of HFSs. We also use line radiative transfer modeling to produce synthetic molecular-line observations and examine how the same structures appear in projected PPV data. In our simulation, we find that 80% of future massive stars are associated with clustered environments. Their growth is also highly episodic: typically, about 40% of the accreted mass is gained during periods of enhanced accretion that occupy only about 10% of the total growth time. Periods of enhanced accretion occur slightly closer to three-dimensional HFS proxies, suggesting a possible link between HFS morphology and episodic accretion in future massive stars. Overall, our results suggest that the early growth of future massive stars is connected to both their clustered environment and the HFS structure of the surrounding gas, and projection effects must be considered when interpreting HFS in PPV data.
Comments15 pages, 9 figures, 1 table
