恒星形成的动力学和结果与喷流、辐射、风和超新星的一致
The dynamics and outcome of star formation with jets, radiation, winds, and supernovae in concert
摘要：
我们分析了第一个巨大的分子云（GMC）的模拟，以遵循个别恒星的形成和他们的反馈，从喷流，辐射，风和超新星，使用STARFORGE框架的GIZMO代码。我们发展的GMC为$\sim 9 \rm Myr$，从最初的湍流崩溃分散反馈。原恒星喷流最初主导反馈动量，但辐射和风导致$\sim 8\%$恒星形成效率（SFE）的云中断，而$8.3 \rm Myr$的第一颗超新星来得太晚，无法显著影响恒星形成。每次自由落体的SFE是动态的，在快速下降到<1%之前从0加速到$\sim 18\%$，但是YSO计数的估计将其压缩到更窄的范围。主星团形成等级，并凝聚成一个简短的（$\sim 1\,\mathrm{Myr}$）紧凑（$\sim 1 \rm pc$）阶段，但在云分散之前不会维里化，恒星最终成为一个无约束的膨胀星协。初始质量函数类似于Chabrier（2005）的形式，具有高质量斜率$α=-2$和最大质量$55 M_\odot$。恒星吸积平均需要$\sim 400 \rm kyr$，但$>10 M_\odot$恒星需要$\gtrsim 1\rm Myr$，因此大质量恒星最晚完成生长。正如观测到的那样，恒星在倍数中所占的比例随着初始质量的增加而增加。总的来说，与完全忽略不同反馈物理的变体相比，模拟更接近现实。但是，更详细的比较与合成观测是必要的，以限制理论的不确定性。
英文摘要：
We analyze the first giant molecular cloud (GMC) simulation to follow the formation of individual stars and their feedback from jets, radiation, winds, and supernovae, using the STARFORGE framework in the GIZMO code. We evolve the GMC for $\sim 9 \rm Myr$, from initial turbulent collapse to dispersal by feedback. Protostellar jets dominate feedback momentum initially, but radiation and winds cause cloud disruption at $\sim 8\%$ star formation efficiency (SFE), and the first supernova at $8.3 \rm Myr$ comes too late to influence star formation significantly. The per-freefall SFE is dynamic, accelerating from 0 to $\sim 18\%$ before dropping quickly to <1%, but the estimate from YSO counts compresses it to a narrower range. The primary cluster forms hierarchically and condenses to a brief ($\sim 1\,\mathrm{Myr}$) compact ($\sim 1 \rm pc$) phase, but does not virialize before the cloud disperses, and the stars end as an unbound expanding association. The initial mass function resembles the Chabrier (2005) form with a high-mass slope $α=-2$ and a maximum mass of $55 M_\odot$. Stellar accretion takes $\sim 400 \rm kyr$ on average, but $\gtrsim 1\rm Myr$ for $>10 M_\odot$ stars, so massive stars finish growing latest. The fraction of stars in multiples increases as a function of primary mass, as observed. Overall, the simulation much more closely resembles reality, compared to variations which neglect different feedback physics entirely. But more detailed comparison with synthetic observations is necessary to constrain the theoretical uncertainties.
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