NUMERICAL SIMULATIONS OF TURBULENT MOLECULAR CLOUDS REGULATED BY RADIATION FEEDBACK FORCES. I. STAR FORMATION RATE AND EFFICIENCY
NUMERICAL SIMULATIONS OF TURBULENT MOLECULAR CLOUDS REGULATED BY RADIATION FEEDBACK FORCES. I. STAR FORMATION RATE AND EFFICIENCY
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由辐射反馈力调节的湍流分子云的数值模拟。
DOI：
10.3847/0004-637x/829/2/130
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
M. A. Skinner
中科院分区：
文献类型：
--
作者：
S. Raskutti;E. Ostriker;M. A. Skinner
来自星团的辐射反馈有望在决定巨型分子云中恒星形成的速度和效率方面发挥关键作用。为了研究辐射力如何影响现实的湍流系统，我们使用Hyperion辐射流体动力学解算器进行了一系列数值模拟，考虑了光学厚度到紫外线和光学厚度到红外辐射的区域。我们的模型云覆盖了初始表面密度之间，具有不同的初始湍流。我们跟随它们经历了湍流、自引力崩塌、星团形成和星云通过恒星辐射扩散的过程。我们的所有模型都表现出气体表面密度Σ的对数正态分布；对于初始维里参数，对数正态标准差IS和恒星形成率系数都对湍流敏感，但对辐射反馈不敏感。净星形成效率(SFE)随温度的升高而增大，随温度的增大而减小。我们通过一个简单的概念框架来解释这些结果，即稳定的恒星形成增加了辐射力，使得连续较高Σ的局部气体斑块变得不受约束。基于这种形式(在固定的情况下)，我们给出了一个解析上界，这与我们的数值结果很好地吻合。最终的超临界流体能量依赖于云中爱丁顿比的分布，并受到气体湍流压缩的强烈影响。
Radiation feedback from stellar clusters is expected to play a key role in setting the rate and efficiency of star formation in giant molecular clouds. To investigate how radiation forces influence realistic turbulent systems, we have conducted a series of numerical simulations employing the Hyperion radiation hydrodynamics solver, considering the regime that is optically thick to ultraviolet and optically thin to infrared radiation. Our model clouds cover initial surface densities between , with varying initial turbulence. We follow them through turbulent, self-gravitating collapse, star cluster formation, and cloud dispersal by stellar radiation. All our models display a log-normal distribution of gas surface density Σ; for an initial virial parameter , the log-normal standard deviation is and the star formation rate coefficient , both of which are sensitive to turbulence but not radiation feedback. The net star formation efficiency (SFE) increases with and decreases with . We interpret these results via a simple conceptual framework, whereby steady star formation increases the radiation force, such that local gas patches at successively higher Σ become unbound. Based on this formalism (with fixed ), we provide an analytic upper bound on , which is in good agreement with our numerical results. The final SFE depends on the distribution of Eddington ratios in the cloud and is strongly increased by the turbulent compression of gas.
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影响因子：
4.8
作者：
J. Dale;B. Ercolano;I. Bonnell
通讯作者：
J. Dale;B. Ercolano;I. Bonnell
影响因子：
4.8
作者：
S. Walch;T. Naab
通讯作者：
S. Walch;T. Naab
了解分子云中的恒星形成 - I 视线污染对柱密度结构的影响
影响因子：
6.5
作者：
Schneider N;Ossenkopf V;Csengeri T;Klessen;Federrath
通讯作者：
Federrath
一种根据 2D 观测重建 3D 物理场方差的方法：应用于星际介质中的湍流
DOI：
10.1111/j.1365-2966.2009.16215.x
发表时间：
2010
影响因子：
4.8
作者：
Brunt C
通讯作者：
Brunt C