论文标题

恒星形成的动力和结局与喷气式,辐射,风和超新星音乐会

The dynamics and outcome of star formation with jets, radiation, winds, and supernovae in concert

论文作者

Grudić, Michael Y., Guszejnov, Dávid, Offner, Stella S. R., Rosen, Anna L., Raju, Aman N., Faucher-Giguère, Claude-André, Hopkins, Philip F.

论文摘要

我们使用Gizmo代码中的Starforge框架分析了第一个巨型分子云(GMC)模拟,以遵循单个恒星的形成及其从喷气机,辐射,风和超新星的反馈。我们以$ \ sim 9 \ rm Myr $从初始湍流崩溃到通过反馈分散的方式进化了GMC。原始喷气机最初占据了反馈势头,但是辐射和风在$ \ sim 8 \%$ $ star构造效率(SFE)和第一个超新星$ 8.3 \ rm myr $ $ 8.3 \ rm Myr $中的云破坏太晚,无法显着影响恒星形成。释放sfe是动态的,从0加速到$ \ sim 18 \%$,然后迅速下降到<1%,但YSO的估计值将其压缩到较窄的范围。主簇形成层次,并凝结为简短的($ \ sim 1 \,\ mathrm {myr} $)compact($ \ sim 1 \ rm pc $)阶段,但不会在云分散之前病毒,而恒星则以无界扩展的关联结束。初始质量函数类似于Chabrier(2005)形式,具有高质量斜率$α= -2 $,最大质量为$ 55 m_ \ odot $。恒星积聚的平均价格为$ \ sim 400 \ rm kyr $,但$ \ gtrsim 1 \ rm myr $ $>> 10 m_ \ odot $ stars,因此大量的恒星最新成长。如观察到的那样,倍数中恒星的比例随着原发性质量的函数而增加。总体而言,与完全忽略不同反馈物理的变化相比,模拟更像现实。但是,对于限制理论不确定性,必须进行更详细的比较与合成观察结果。

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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