论文标题
通过细丝的密度扩增统一的低质量和高质量恒星形成
Unifying low and high mass star formation through density amplified hubs of filaments
论文作者
论文摘要
上下文：恒星形成发生在巨大的分子云中，导致质量分离的年轻恒星簇由阳光状的恒星，棕色矮人和巨大的O型（50-100 \ msun）恒星组成。目的：鉴定牛奶路中的候选枢纽丝系统（HFS），并检查它们在最高质量恒星和恒星簇的形成中的作用。方法：使用分散算法检测到的〜35000个higal块的细丝。集线器定义为三个或三个或更多细丝的连接。用细丝骨骼掩盖了柱密度图，并为HFS和非HFS样品平均，以将沿着灯丝沿着团块计算的径向轮廓。结果：〜3700〜（11 \％）是候选HF，其中〜2150〜（60 \％）是前遗迹，〜1400〜（40 \％）是原始的。所有具有L> 10^4 lsun和L> 10^5 lsun的团块分别在2kpc和5kpc之内，位于HFS的枢纽中。发现轮毂的柱密度通过〜2（前恒星源）的增强（原始词来源）增强。结论：所有高质量恒星优先形成HFS的密度增强的枢纽。这种扩增可以驱动观察到的沿细丝的纵向流，从而提供进一步的质量积聚。辐射压力和反馈可以逃脱到丝虫间空隙中。 We propose a "filaments to clusters" unified paradigm for star formation, with the following salient features: a) low-intermediate mass stars form in the filaments slowly (10^6yr) and massive stars quickly (10^5yr) in the hub, b) the initial mass function is the sum of stars continuously created in the HFS with all massive stars formed in the hub, c) Feedback dissiption and mass segregation arise naturally由于HFS性质，以及c）解释在结合簇内的年龄差，并形成孤立的OB关联。
Context: Star formation takes place in giant molecular clouds, resulting in mass-segregated young stellar clusters composed of Sun-like stars, brown dwarves, and massive O-type(50-100\msun) stars. Aims: To identify candidate hub-filament systems (HFS) in the Milky-Way and examine their role in the formation of the highest mass stars and star clusters. Methods: Filaments around ~35000 HiGAL clumps that are detected using the DisPerSE algorithm. Hub is defined as a junction of three or more filaments. Column density maps were masked by the filament skeletons and averaged for HFS and non-HFS samples to compute the radial profile along the filaments into the clumps. Results: ~3700~(11\%) are candidate HFS of which, ~2150~(60\%) are pre-stellar, ~1400~(40\%) are proto-stellar. All clumps with L>10^4 Lsun and L>10^5 Lsun at distances respectively within 2kpc and 5kpc are located in the hubs of HFS. The column-densities of hubs are found to be enhanced by a factor of ~2 (pre-stellar sources) up to ~10 (proto-stellar sources). Conclusions: All high-mass stars preferentially form in the density enhanced hubs of HFS. This amplification can drive the observed longitudinal flows along filaments providing further mass accretion. Radiation pressure and feedback can escape into the inter-filamentary voids. We propose a "filaments to clusters" unified paradigm for star formation, with the following salient features: a) low-intermediate mass stars form in the filaments slowly (10^6yr) and massive stars quickly (10^5yr) in the hub, b) the initial mass function is the sum of stars continuously created in the HFS with all massive stars formed in the hub, c) Feedback dissiption and mass segregation arise naturally due to HFS properties, and c) explain age spreads within bound clusters and formation of isolated OB associations.
