早期宇宙中的分子氟化学
Molecular fluorine chemistry in the early Universe
摘要：
大爆炸核合成的一些模型表明，在早期宇宙中形成了非常高的重子密度区域，并产生了除锂以外的重元素，如氟F。我们提出了一个全面的化学氟在后复合时代。计算F，F-和HF的丰度，作为红移z的函数，进行。主要结果是，早期宇宙的化学条件可以导致HF的形成。当中性氟的初始丰度为10（-15）时，双原子分子HF的最终丰度接近3.75 10（-17）。这些结果表明，氟HF分子在黑暗时代已经存在。这可能对原始物体的演化和宇宙微波背景辐射的各向异性产生影响。氟的氢化物HF可能影响来自原始物体的发射线强度的增强，并且可能产生光谱-空间波动。
英文摘要：
Some models of Big Bang nucleosynthesis suggest that very high baryon density regions were formed in the early Universe, and generated the production of heavy elements other than lithium such as fluorine F. We present a comprehensive chemistry of fluorine in the post-recombination epoch. Calculation of F, F- and HF abundances, as a function of redshift z, are carried out. The main result is that the chemical conditions in the early Universe can lead to the formation of HF. The final abundance of the diatomic molecule HF is predicted to be close to 3.75 10(-17) when the initial abundance of neutral fluorine F is 10(-15). These results indicate that molecules of fluorine HF were already present during the dark age. This could have implications on the evolution of proto-objects and on the anisotropies of cosmic microwave background radiation. Hydride of fluorine HF may affect enhancement of the emission line intensity from the proto-objects and could produce spectral-spatial fluctuations.
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