Standard Big-Bang Nucleosynthesis after Planck
Standard Big-Bang Nucleosynthesis after Planck
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普朗克之后的标准大爆炸核合成
DOI：
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
E. Vangioni
中科院分区：
文献类型：
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作者：
A. Coc;J. Uzan;E. Vangioni
原始核合成（BBN）与宇宙膨胀和宇宙微波背景辐射（CMB）一起，是大爆炸模型的三大有力证据之一。最近的结果由普朗克使命已经稍微改变了重子密度Ω_B的估计，与以前的WMAP值相比。本文利用普朗克测定的新的Omega_B值、改进的核网络和新的光谱观测，更新了轻元素的BBN预言。虽然没有重大修改，但原始D/H丰度（2.67+/-0.09）x 10^{-5}的误差条较窄，原始Li/H丰度（4.89^+0.41_-0.39）x 10^{-10}略有降低。然而，最后一个值仍然比在银河系晕星中观察到的光谱丰度大~3倍。原始氦丰度为Y_p = 0.2463+/-0.0003。
Primordial or Big Bang nucleosynthesis (BBN) is one of the three historical strong evidences for the Big-Bang model together with the expansion of the Universe and the Cosmic Microwave Background radiation (CMB). The recent results by the Planck mission have slightly changed the estimate of the baryonic density Omega_b, compared to the previous WMAP value. This article updates the BBN predictions for the light elements using the new value of Omega_b determined by Planck, as well as an improvement of the nuclear network and new spectroscopic observations. While there is no major modification, the error bars of the primordial D/H abundance (2.67+/-0.09) x 10^{-5} are narrower and there is a slight lowering of the primordial Li/H abundance (4.89^+0.41_-0.39) x 10^{-10}. However, this last value is still ~3 times larger than its observed spectroscopic abundance in halo stars of the Galaxy. Primordial Helium abundance is now determined to be Y_p = 0.2463+/-0.0003.