Title: Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence Show Chinese title

Title: 高质量恒星盘风反馈。 Ⅱ. 演化序列

Abstract: Star formation is ubiquitously associated with the ejection of accretion-powered outflows that carve bipolar cavities through the infalling envelope. This feedback is expected to be important for regulating the efficiency of star formation from a natal pre-stellar core. These low-extinction outflow cavities greatly affect the appearance of a protostar by allowing the escape of shorter wavelength photons. Doppler-shifted CO line emission from outflows is also often the most prominent manifestation of deeply embedded early-stage star formation. Here, we present 3D magneto-hydrodynamic simulations of a disk wind outflow from a protostar forming from an initially $60\:M_\odot$ core embedded in a high pressure environment typical of massive star-forming regions. We simulate the growth of the protostar from $m_*=1\:M_\odot$ to $26\:M_\odot$ over a period of $\sim$100,000 years. The outflow quickly excavates a cavity with half opening angle of $\sim10^\circ$ through the core. This angle remains relatively constant until the star reaches $4\:M_\odot$. It then grows steadily in time, reaching a value of $\sim 50^\circ$ by the end of the simulation. We estimate a lower limit to the star formation efficiency (SFE) of 0.43. However, accounting for continued accretion from a massive disk and residual infall envelope, we estimate that the final SFE may be as high as $\sim0.7$. We examine observable properties of the outflow, especially the evolution of the cavity opening angle, total mass and momentum flux, and velocity distributions of the outflowing gas, and compare with the massive protostars G35.20-0.74N and G339.88-1.26 observed by ALMA, yielding constraints on their intrinsic properties. Show Chinese abstract

Abstract: 恒星形成普遍伴随着吸积功率驱动的喷流的喷射，这些喷流通过吸积包层雕刻出双极空腔。 这种反馈预计对于调节从母体先恒星核中恒星形成的效率非常重要。 这些低消光的喷流空腔通过允许短波长光子逃逸，极大地影响了原恒星的外观。 来自喷流的 Doppler 位移 CO 线发射也通常是早期嵌入阶段恒星形成的最显著表现。 在这里，我们展示了从一个最初嵌入于高压力环境（典型于大质量恒星形成区域）的 $60\:M_\odot$核心中形成的原恒星盘风喷流的三维磁流体力学模拟。 我们模拟了原恒星在 $m_*=1\:M_\odot$到 $26\:M_\odot$的增长过程，持续时间为 $\sim$的 100,000 年。 喷流迅速在核心中挖出一个半张角为 $\sim10^\circ$的空腔。 这个角度在恒星达到 $4\:M_\odot$之前相对保持不变。 之后它随着时间逐渐增大，在模拟结束时达到 $\sim 50^\circ$。 我们估计恒星形成效率（SFE）的下限为 0.43。 然而，考虑到吸积盘持续吸积以及剩余塌缩包层的影响，我们估计最终的 SFE 可能高达$\sim0.7$。 我们检查了外流的可观测属性，特别是腔体张开角度、总质量和动量通量以及外流气体速度分布的演化，并与 ALMA 观测到的大质量原恒星 G35.20-0.74N 和 G339.88-1.26 进行比较，从而对其固有性质施加限制。