Constraining the astrophysical origin of the p-nuclei through nuclear physics and meteoritic data
Constraining the astrophysical origin of the p-nuclei through nuclear physics and meteoritic data
复制标题
DOI：
10.1088/0034-4885/76/6/066201
复制
发表时间：
2013-03
影响因子：
18.1
通讯作者：
T. Rauscher;T. Rauscher;T. Rauscher;Nicolas Dauphas;I. Dillmann;Carla Fröhlich;Z. Fülöp;G. Gyürky
中科院分区：
文献类型：
--
作者：
T. Rauscher;T. Rauscher;T. Rauscher;Nicolas Dauphas;I. Dillmann;Carla Fröhlich;Z. Fülöp;G. Gyürky
少数自然产生的富含质子的核素（p核）不能在s-和r-过程中产生。它们的起源还不太清楚。大质量恒星可以通过光致蜕变产生p核，这种蜕变是由已经存在的中重核和重核完成的。这种所谓的γ过程需要很高的恒星等离子体温度，主要发生在核心坍缩超新星的O/Ne爆炸燃烧中。虽然大质量恒星中的γ过程已经成功地产生了大量的p核，但仍然存在重大的缺陷。近年来，为了寻找替代或补充大质量星星模型的可行方案，对越来越多的过程和地点进行了研究。然而，大量的不稳定核，只有理论预测的反应速率被包括在反应网络中，因此核输入也可能具有相当大的不确定性。评述了天体物理模型、核输入和观测约束的现状。在概述了目前讨论的模型之后，重点是通过不同手段更好地约束这些模型的可能性。陨石数据不仅提供了p核的实际同位素丰度，而且还可以限制富质子核合成的可能贡献。审查的主要部分集中在核合成研究中使用的扩展反应网络所需的天体物理反应速率的确定所涉及的核不确定性。实验方法进行了讨论，连同其必要的连接到理论，这是特别明显的反应与中间和重核爆炸性核燃烧，甚至接近稳定。
A small number of naturally occurring, proton-rich nuclides (the p-nuclei) cannot be made in the s- and r-processes. Their origin is not well understood. Massive stars can produce p-nuclei through photodisintegration of pre-existing intermediate and heavy nuclei. This so-called γ-process requires high stellar plasma temperatures and occurs mainly in explosive O/Ne burning during a core-collapse supernova. Although the γ-process in massive stars has been successful in producing a large range of p-nuclei, significant deficiencies remain. An increasing number of processes and sites has been studied in recent years in search of viable alternatives replacing or supplementing the massive star models. A large number of unstable nuclei, however, with only theoretically predicted reaction rates are included in the reaction network and thus the nuclear input may also bear considerable uncertainties. The current status of astrophysical models, nuclear input and observational constraints is reviewed. After an overview of currently discussed models, the focus is on the possibility to better constrain those models through different means. Meteoritic data not only provide the actual isotopic abundances of the p-nuclei but can also put constraints on the possible contribution of proton-rich nucleosynthesis. The main part of the review focuses on the nuclear uncertainties involved in the determination of the astrophysical reaction rates required for the extended reaction networks used in nucleosynthesis studies. Experimental approaches are discussed together with their necessary connection to theory, which is especially pronounced for reactions with intermediate and heavy nuclei in explosive nuclear burning, even close to stability.