爆发性分子外流
Explosive Molecular Outflows
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中文总结 AI 辅助
研究确认了与极亮大质量年轻星团相关的爆发性分子外流，其与经典双极原恒星流不同，有独特空间分布和膨胀运动。最新理论模型认为其可能由非层级大质量原恒星系统破坏产生。
中文摘要 AI 辅助
大约十五年前，一种与极亮（≥10^5 L⊙）且大质量（10^3 M⊙）年轻星团相关的新型极端（动能 Ek ∼ 10^47 - 49 erg）分子外流——爆发性分子外流被确认。这类外流与经典双极原恒星流大不相同，其空间分布由众多狭窄的直丝状或流光状喷射组成，呈几乎各向同性排列且有明显的类似哈勃 - 勒梅特的膨胀运动。直丝直接指向膨胀的分子或电离壳层中心，壳层膨胀速度约为10 - 50 km s^-1。然而，那里没有明显的年轻大质量恒星，可能是因为它们已移动到其他地方。这些物理特征表明爆发性外流本质上是短暂的，可能由一次高能的单一且短暂的破坏事件产生。最新的解释其本质的理论模型涉及非层级大质量原恒星系统的破坏，其中成员可能形成紧密双星（间距几au）或合并成一颗大质量恒星，如最近针对最近的高质量恒星形成区域猎户座BN/KL所提议的那样。
英文摘要
About fifteen years ago a new type of extreme (with kinetic energies of $\mathrm{E}_k \sim 10^{47-49}\, \mathrm{erg}$) molecular outflows associated with very luminous ($\geq 10^5\, \mathrm{L}_\odot$) and massive (10$^3$ M$_\odot$) young clusters was confirmed, the Explosive Molecular Outflows. This new class of outflows is largely different from the classical bipolar protostellar flows, with spatial distributions made of numerous narrow straight filament- or streamer-like ejections in an almost isotropic arrangement and with clear Hubble--Lemaître-like expansion motions. Straight filaments point directly to the center of expanding molecular or ionized shells, which exhibit expansion velocities of about 10--50 km s$^{-1}$. However, no young massive stars are clearly located there, probably because they moved to other places. These physical characteristics suggest that explosive outflows are short-lived in nature and possibly generated by an energetic single and brief disrupting event. The most up-to-date theoretical model for explaining their nature involves the disruption of non-hierarchical massive protostellar systems, where members may either form a close binary (with separations of a few au) or merge into a single massive star, as recently proposed for the nearest high-mass star-forming region, Orion BN/KL.
