H3+ IN THE EARLY UNIVERSE

Yu-Shan Chen, T. Oka
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Abstract

The chemistry, and radiative and collisional interactions of H3 in the early Universe are examined. The object of study is to investigate whether H3 is essential in cooling of the primordial gas and thus in the formation of the first stars. The consensus so far is overwhelmingly negative. Most previous papers ignore the possibility at the onset because of the very low concentration of H3 , about 10 −9 of H2 or less. Since the dipole infrared emission of H3 is (λ/a) 2 ∼ 10 (λ wavelength: a molecular size) times faster than the quadrupole emission of H2, however, there is a possibility that H3 is comparably efficient coolant as H2. Glover and Savina was the only paper which took this possibility into account. They negate the contribution of H3 because at a gas density higher than 10 cm−3 H3 number density is further reduced by endothermic reaction H + 3 + H → H2 + H + 2 . We will examine this. We will consider the following two effects which have been neglected by the previous workers: (1) the effect of collision which convert translational energy of the gas into the energy of vibration and rotation of the molecules and (2) the effect of spontaneous emission between rotational levels. We find H3 can be a more efficient coolant than H2 in the early Universe depending on temperature, density, and cosmological conditions of the primordial gas at the time of star formation.
早期宇宙中的H3+
研究了早期宇宙中H3的化学、辐射和碰撞相互作用。研究的目的是研究H3在原始气体的冷却和第一批恒星的形成中是否必不可少。迄今为止的共识是压倒性的负面。由于H3的浓度非常低,约为H2的10−9倍或更少,因此大多数先前的论文在开始时忽略了这种可能性。然而,由于H3的偶极子红外发射比H2的四极子发射快(λ/a) 2 ~ 10倍(λ波长:分子大小),因此有可能H3是与H2相当有效的冷却剂。格洛弗和萨维娜是唯一一篇考虑到这种可能性的论文。它们抵消了H3的贡献,因为当气体密度大于10 cm−3时,H3数密度通过吸热反应H + 3 + H→H2 + H + 2进一步降低。我们将对此进行研究。我们将考虑以下两个以前的工作者所忽略的影响:(1)碰撞的影响,它将气体的平动能量转化为分子的振动和旋转能量;(2)旋转能级之间的自发发射的影响。我们发现H3在早期宇宙中是比H2更有效的冷却剂,这取决于恒星形成时原始气体的温度、密度和宇宙条件。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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