The Mass of the First Stars
The Mass of the First Stars
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第一批恒星的质量
DOI：
10.1088/0004-637x/773/2/185
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发表时间：
2013
期刊：
影响因子：
--
通讯作者：
Hajime Susa
中科院分区：
文献类型：
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作者：
Tazaki;F.;Ueda;Y. et al;Hajime Susa
我们进行了一个三维辐射流体动力学模拟研究的第一批恒星的形成，从最初的原始气体云的崩溃的形成和原恒星的生长。这个模拟一直持续到主原恒星形成后100万年，此时原恒星已经在主序星上稳定下来。这项工作是第一次尝试模拟的第一集的星星形成，考虑到紫外线辐射反馈效应从多个原恒星以及三维效应的碎片的吸积盘。我们发现，到人口III原恒星的质量吸积显着抑制其辐射反馈。结果，我们发现在这个特殊的模拟中形成了五颗恒星。恒星的最终质量为1060 M，包括一颗4.4 M的星星。这样一颗星星的形成暗示了今天存在的质量更低的恒星的存在。
We perform a three-dimensional radiation hydrodynamics simulation to investigate the formation of the first stars from the initial collapse of a primordial gas cloud to the formation and growth of protostars. The simulation is integrated until∼ 0.1 Myr after the formation of the primary protostar, by which time the protostars have already settled onto the main sequence. This work represents the first attempt at simulating the first episodes of star formation, taking into account the ultraviolet radiative feedback effect from multiple protostars as well as the three-dimensional effects of the fragmentation of the accretion disk. We find that the mass accretion onto Population III protostars is significantly suppressed by their radiative feedback. As a result, we find five stars formed in this particular simulation. The final masses of the stars are≲ 60 M☉, including a star of 4.4 M☉. Formation of such a star hints at the existence of even lower-mass stars that would live today.