论文标题
h $ _3 $的rydberg州和heh作为原始星形形成的潜在冷却剂
Rydberg States of H$_3$ and HeH as Potential Coolants for Primordial Star Formation
论文作者
论文摘要
当前的理论和测量值确定了宇宙的年龄。 138亿年。在其存在的前几亿年中，它是一个黑暗的不透明的空白。此后，包括大多数“普通”物质的氢原子开始凝结和电离，最终形成了第一批照亮天空的恒星。这些“原始”恒星如何形成的细节已广泛争论，但仍然难以捉摸。在此过程中的一个核心问题是通过暗物质冷却的作用并进一步吸收融合密度的原始气体（主要是氢和氦原子）的机制。当前的模型调用了h $ _2 $分子旋转的碰撞激发以及弱分子四极力矩允许的辐射旋转转变。在本文中，我们回顾了有关中性h $ _3 $ rydberg电子状态在中红外的近期光谱观察结果的显着考虑因素，并提出了一些新想法。
Current theory and measurements establish the age of the universe as ca. 13.8 billion years. For the first several hundred million years of its existence, it was a dark, opaque void. After that, the hydrogen atoms comprising most of the "ordinary" matter began to condense and ionize, eventually forming the first stars that would illuminate the sky. Details of how these "primordial" stars formed have been widely debated, but remain elusive. A central issue in this process is the mechanism by which the primordial gas (mainly hydrogen and helium atoms) collected via the action of dark matter cools and further accretes to fusion densities. Current models invoke collisional excitation of H$_2$ molecular rotations and subsequent radiative rotational transitions allowed by the weak molecular quadrupole moment. In this article, we review the salient considerations, and present some new ideas, bases on recent spectroscopic observations of neutral H$_3$ Rydberg electronic state emission in the mid-infrared.
