追踪氘的后BBN演化
Tracking The Post-BBN Evolution Of Deuterium
摘要：
在大爆炸核合成（BBN）过程中产生的氘的原始丰度敏感地依赖于重子与光子的普适比，这是一个重要的宇宙学参数，由宇宙微波背景（CMB）辐射独立探测。在高红移、低金属量的类星体吸收线系统（QSOALS）中对氘的观测提供了一个关键的气压计，它可以确定BBN时的重子丰度，精确度为5%。或者，如果在BBN计算原始丰度时使用CMB确定的重子光子比，BBN预测的氘丰度可以与从QSOALS推断的原始值进行比较，测试标准宇宙学模型。在后BBN宇宙中，当气体在恒星中循环时，氘只会被破坏，因此它的丰度在宇宙中的任何地方都可以测量，从下面限制了原始丰度。后BBN银河系化学演化模型的限制遵循的遗迹氘丰度与FUSE推断的氘丰度在化学富集，恒星处理的材料的本地ISM的比较。
英文摘要：
The primordial abundance of deuterium produced during Big Bang Nucleosynthesis (BBN) depends sensitively on the universal ratio of baryons to photons, an important cosmological parameter probed independently by the Cosmic Microwave Background (CMB) radiation. Observations of deuterium in high-redshift, low-metallicity QSO Absorption Line Systems (QSOALS) provide a key baryometer, determining the baryon abundance at the time of BBN to a precision of 5%. Alternatively, if the CMB-determined baryon to photon ratio is used in the BBN calculation of the primordial abundances, the BBN-predicted deuterium abundance may be compared with the primordial value inferred from the QSOALS, testing the standard cosmological model. In the post-BBN universe, as gas is cycled through stars, deuterium is only destroyed so that its abundance measured anytime, anywhere in the Universe, bounds the primordial abundance from below. Constraints on models of post-BBN Galactic chemical evolution follow from a comparison of the relic deuterium abundance with the FUSE-inferred deuterium abundances in the chemically enriched, stellar processed material of the local ISM.
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