Disruption of giant molecular clouds and formation of bound star clusters under the influence of momentum stellar feedback
Disruption of giant molecular clouds and formation of bound star clusters under the influence of momentum stellar feedback
复制标题
动量恒星反馈影响下巨分子云的破裂和束缚星团的形成
DOI：
10.1093/mnras/stz1271
复制
发表时间：
2019
影响因子：
4.8
通讯作者：
Gnedin, Oleg Y
中科院分区：
文献类型：
--
作者：
Li, Hui;Vogelsberger, Mark;Marinacci, Federico;Gnedin, Oleg Y
来自星星团的能量反馈在形成巨分子云的动力学演化过程中起着至关重要的作用。为了研究恒星反馈对云的星星形成效率和嵌入的星星团的动力学响应的影响，我们使用动网格流体动力学程序Arepo对星星形成和动量反馈亚网格模型进行了一系列孤立的GMC模拟。我们模拟的GMCs的性质跨越了广泛的初始质量，半径和速度配置。我们发现，最终的恒星质量的总质量的比率，云，dielint，规模强烈的初始云表面密度和动量反馈强度。这种相关性解释了一个分析模型，认为重力和动量反馈之间的力平衡。对于所有模拟的GMC，恒星密度剖面系统陡峭的比气体的星星形成的高峰时期，这表明一个集中的恒星分布。我们还发现，星星总是处于亚维里状态的维里参数为<$0.6之前的气体驱逐。亚维里动力学状态和陡峭的恒星密度分布都阻止了星团在其演化的气体去除阶段的分散。最后的集群绑定分数是一个不断增加的函数的xlint。星星形成效率小于0.5的GMC仍然能够形成具有大束缚分数的团簇。
Energetic feedback from star clusters plays a pivotal role in shaping the dynamical evolution of giant molecular clouds (GMCs). To study the effects of stellar feedback on the star formation efficiency of the clouds and the dynamical response of embedded star clusters, we perform a suite of isolated GMC simulations with star formation and momentum feedback subgrid models using the moving-mesh hydrodynamics codeArepo. The properties of our simulated GMCs span a wide range of initial mass, radius, and velocity configurations. We find that the ratio of the final stellar mass to the total cloud mass, ϵint, scales strongly with the initial cloud surface density and momentum feedback strength. This correlation is explained by an analytic model that considers force balancing between gravity and momentum feedback. For all simulated GMCs, the stellar density profiles are systematically steeper than that of the gas at the epochs of the peaks of star formation, suggesting a centrally concentrated stellar distribution. We also find that star clusters are always in a sub-virial state with a virial parameter ∼0.6 prior to gas expulsion. Both the sub-virial dynamical state and steeper stellar density profiles prevent clusters from dispersal during the gas removal phase of their evolution. The final cluster bound fraction is a continuously increasing function of ϵint. GMCs with star formation efficiency smaller than 0.5 are still able to form clusters with large bound fractions.
登录
查看更多内容
模拟大质量恒星的紫外线辐射反馈。
DOI：
10.3847/1538-4357/aabe27
发表时间：
2018
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Kim, Jeong-Gyu;Kim, Woong-Tae;Ostriker, Eve C.
通讯作者：
Ostriker, Eve C.
影响因子：
6.5
作者：
Nina Brinkmann;S. Banerjee;Bhawna Motwani;P. Kroupa
通讯作者：
Nina Brinkmann;S. Banerjee;Bhawna Motwani;P. Kroupa
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
发表时间：
2016
期刊：
The Astrophysical Journal
影响因子：
--
作者：
S. Raskutti;E. Ostriker;M. A. Skinner
通讯作者：
M. A. Skinner
恒星形成区恒星结构的动力学状态
DOI：
10.1111/j.1365-2966.2011.19748.x
发表时间：
2011
影响因子：
4.8
作者：
J. Kruijssen;T. Maschberger;N. Moeckel;C. Clarke;N. Bastian;Ian A. Bonnell Utrecht;Leiden;Mpa Garching;I. Cambridge;Bonn;Grenoble;Excellence Cluster Munich;S. Andrews
通讯作者：
S. Andrews
影响因子：
64.8
作者：
M. Vogelsberger;S. Genel;V. Springel;P. Torrey;D. Sijacki;Da Xu;G. Snyder;Simeon Bird;D. Nelson;Lars Hernquist Mit;HarvardCfA;Hits;I. Cambridge;Stsci;Ias Princeton
通讯作者：
M. Vogelsberger;S. Genel;V. Springel;P. Torrey;D. Sijacki;Da Xu;G. Snyder;Simeon Bird;D. Nelson;Lars Hernquist Mit;HarvardCfA;Hits;I. Cambridge;Stsci;Ias Princeton