Radiative Feedback from Primordial Protostars and Final Mass of the First Stars
Radiative Feedback from Primordial Protostars and Final Mass of the First Stars
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来自原始原恒星的辐射反馈和第一颗恒星的最终质量
DOI：
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发表时间：
2012
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影响因子：
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通讯作者：
H. Yorke
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作者：
T. Hosokawa;K. Omukai;N. Yoshida;H. Yorke
在这篇文章中，我们回顾了我们为理解原始恒星的典型质量尺度所做的努力。我们的直接数值模拟表明，在星族III.1和III.2的情况下，强烈的紫外线恒星辐射反馈终止了原恒星的质量吸积。在原恒星周围形成的HII区域非常动态地扩展到吸积包膜中，并切断了对星周盘的气体供应。圆盘暴露在恒星的紫外线辐射下，通过光蒸发失去质量。在我们的基准星族III.1和III.2的情况下，导出的最终质量分别为43 M⊙和17 M⊙。然而，更大质量的恒星应该在其他特殊条件下形成。例如，在H2分子解离的原子冷却晕中，原恒星通过非常快速的质量吸积生长，速率为M* ~ 0.1 ~ 1m⊙yr−1。我们新的恒星演化计算表明，在这种情况下，原恒星明显膨胀，从未收缩到零年龄序列阶段。这样的“超级巨人……
In this contribution, we review our efforts toward understanding the typical mass-scale of primordial stars. Our direct numerical simulations show that, in both of Population III.1 and III.2 cases, strong UV stellar radiative feedback terminatesmass accretion onto a protostar. An HII region formed around the protostar expands very dynamically into the accreting envelope, and cuts off the gas supply to a circumstellar disk. The disk is exposed to the stellar UV radiation and loses its mass by photoevaporation. The derived final masses are 43 M⊙ and 17 M⊙ in our fiducial Population III.1 and III.2 cases. Much more massive stars, however, should form in other exceptional conditions. In atomic-cooling halos where H2 molecules are dissociated, for instance, a protostar grows via very rapid mass accretion with the rates M*∼0.1-1M⊙yr−1. Our new stellar evolution calculations show that the protostar significantly inflates and never contracts to reach the zero-agemain-sequence stage in this case. Such "supergiant ...