Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence
Disk Wind Feedback from High-mass Protostars. II. The Evolutionary Sequence
复制标题
DOI：
10.3847/1538-4357/acbd47
复制
发表时间：
2023-01
期刊：
影响因子：
--
通讯作者：
J. Staff;Kei E. I. Tanaka;J. Ramsey;Yichen Zhang;J. Tan
中科院分区：
文献类型：
--
作者：
J. Staff;Kei E. I. Tanaka;J. Ramsey;Yichen Zhang;J. Tan
星星的形成普遍与吸积动力流出物的喷射有关，这些流出物通过下落的包层雕刻出双极腔。这种反馈对于调节纳塔尔星前核形成星星的效率是很重要的。这些低消光外流腔通过允许较短波长的光子逃逸，极大地影响了原恒星的外观。多普勒频移的CO谱线从外流中发射出来，也常常是深埋的早期星星形成的最突出的表现。在这里，我们提出了3D磁流体动力学模拟盘风流出的原恒星形成从最初的60 M的核心嵌入在一个典型的大规模恒星形成区域的高压环境。我们模拟了原恒星从m * = 1 M φ到26 M φ的生长过程，时间为10万年。流出物迅速通过岩心挖出一个半开角为10°的空腔。在星星达到4 M φ之前，这个角度保持相对恒定。然后，它随时间稳定增长，在模拟结束时达到± 50°的值。我们估计星星形成效率（SFE）的下限为0.43。然而，考虑到来自大质量盘的持续吸积和残留的陷落包层，我们估计最终的SFE可能高达0.7。我们检查可观察到的流出，特别是腔的开口角，总质量和动量通量的演变，和流出的气体的速度分布，并与阿塔卡马大型毫米/亚毫米阵列（阿尔马）观察到的大质量原恒星G35.20- 0.74 N和G339.88-1.26进行比较，产生限制其固有特性。
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 prestellar 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 magnetohydrodynamic simulations of a disk wind outflow from a protostar forming from an initially 60 M ⊙ core embedded in a high-pressure environment typical of massive star-forming regions. We simulate the growth of the protostar from m * = 1 M ⊙ to 26 M ⊙ over a period of ∼100,000 yr. The outflow quickly excavates a cavity with a half opening angle of ∼10° through the core. This angle remains relatively constant until the star reaches 4 M ⊙. It then grows steadily in time, reaching a value of ∼50° 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 ∼0.7. We examine observable properties of the outflow, especially the evolution of the cavity's opening angle, total mass, and momentum flux, and the velocity distributions of the outflowing gas, and compare with the massive protostars G35.20-0.74N and G339.88-1.26 observed by the Atacama Large Millimeter/submillimeter Array (ALMA), yielding constraints on their intrinsic properties.