标题： 流出反馈调节的星团形成尺度上的大质量恒星形成 显示英文标题

标题： Outflow Feedback Regulated Massive Star Formation in Parsec-Scale Cluster Forming Clumps

摘要： （摘要）我们研究了包括原恒星外流反馈的湍动、磁化、以秒差距尺度的分子云团块中的大质量恒星形成，使用基于Enzo的包含吸积汇粒子和有效分辨率为$2048^3$的磁流体力学模拟。 我们发现，在没有磁场和外流反馈调节的情况下，大质量恒星容易在由数百个较低质量恒星组成的星团中，在一个包含约$\sim 1,600$倍太阳质量的湍动、适度凝聚的团块中形成。 大质量恒星通过以下两种方式被大量供应物质：(1) 在早期阶段由大规模湍动压缩产生的瞬态密集丝状结构，以及(2) 在晚期阶段由于湍动衰减而引起的整体塌缩。 在这两种情况下，大质量恒星的大部分质量都来自围绕恒星的直径为0.1秒差距大小的“核心”之外。 在我们的模拟中，大质量恒星是由整个团块喂养而不是核心喂养。 这种大规模喂养的需求使得大质量恒星的形成容易受到外流反馈的调节，后者直接对抗喂养过程。 外流通过在早期破坏喂养大质量恒星形成的密集丝状结构，以及在晚期通过集体减缓提供燃料的整体塌缩来减少大质量恒星的质量吸积率。 后一种作用由强度处于观测范围内的适度磁场协助完成。 我们得出结论，我们在模拟的湍动、磁化的秒差距尺度的团块中的大质量恒星形成是受外流调节且由团块喂养的（简称为ORCF）。 一个重要含义是，密集团块中低质量恒星的形成可以通过它们对外流动力学的影响影响同一团块中大质量恒星的形成。 显示英文摘要

摘要： (Abridged) We investigate massive star formation in turbulent, magnetized, parsec-scale clumps of molecular clouds including protostellar outflow feedback using Enzo-based MHD simulations with accreting sink particles and effective resolution $2048^3$. We find that, in the absence of regulation by magnetic fields and outflow feedback, massive stars form readily in a turbulent, moderately condensed clump of $\sim 1,600$ solar masses, along with a cluster of hundreds of lower mass stars. The massive stars are fed at high rates by (1) transient dense filaments produced by large-scale turbulent compression at early times, and (2) by the clump-wide global collapse resulting from turbulence decay at late times. In both cases, the bulk of the massive star's mass is supplied from outside a 0.1 pc-sized "core" that surrounds the star. In our simulation, the massive star is clump-fed rather than core-fed. The need for large-scale feeding makes the massive star formation prone to regulation by outflow feedback, which directly opposes the feeding processes. The outflows reduce the mass accretion rates onto the massive stars by breaking up the dense filaments that feed the massive star formation at early times, and by collectively slowing down the global collapse that fuel the massive star formation at late times. The latter is aided by a moderate magnetic field of strength in the observed range. We conclude that the massive star formation in our simulated turbulent, magnetized, parsec-scale clump is outflow-regulated and clump-fed (ORCF for short). An important implication is that the formation of low-mass stars in a dense clump can affect the formation of massive stars in the same clump, through their outflow feedback on the clump dynamics.