第一颗原恒星周围的高熵极区
High-Entropy Polar Regions Around the First Protostars
摘要：
我们报告了宇宙中第一批恒星形成的模拟，在那里我们识别出密度超过10-14 g/cc的热原子气体（fH 2 < 10-6）区域，加热到3000至8000 K之间的温度。在这个温度范围内，原子氢不能有效地冷却。我们描述了这些地区的动力学和热特性，并调查其起源。我们发现，这些地区，而小的总质量分数的云，可能是动态的重要的吸积时间尺度的云，特别是作为一个化学，而不是辐射，机制清除极地地区的吸积盘的材料和终止吸积沿这些方向。这些固有的三维效应强调需要多维度计算的原恒星吸积可靠的预测质量的第一个恒星。
英文摘要：
We report on simulations of the formation of the first stars in the Universe, where we identify regions of hot atomic gas (fH2 < 10-6) at densities above 10-14 g/cc, heated to temperatures ranging between 3000 and 8000 K. Within this temperature range atomic hydrogen is unable to cool effectively. We describe the kinetic and thermal characteristics of these regions and investigate their origin. We find that these regions, while small in total mass fraction of the cloud, may be dynamically important over the accretion timescale for the central clump in the cloud, particularly as a chemical, rather than radiative, mechanism for clearing the polar regions of the accretion disk of material and terminating accretion along these directions. These inherently three-dimensional effects stress the need for multi-dimensional calculations of protostellar accretion for reliable predictions of the masses of the very first stars.
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