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Stellar matter: supernovae as sources of r-process elements ((17) M06)

恒星物质：超新星作为 r 过程元素的来源 ((17) M06)

基本信息

批准号：
327949753
负责人：
金额：
--
依托单位：
Arbeitsgruppe Nukleare Astrophysik
依托单位国家：
德国
项目类别：
Collaborative Research Centres
财政年份：
2017
资助国家：
德国
起止时间：
2016-12-31 至 2020-12-31
项目状态：
已结题

来源：
https://gepris.dfg.de/gepris/projekt/327949753?language=en
关键词：
Stellar matter supernovae sources process

项目摘要

The rapid neutron capture process (r-process) is the mechanism by which at least half of the elemental abundances greater than iron are produced in the universe. Its site remains unknown and determining where it occurs is one of the most outstanding questions to be answered in nuclear astrophysics. Present theoretical candidate sites are core collapse supernovae (CCSNe) and binary neutron star mergers. Present state of the art 3D supernova models are too computationally expensive to compute outwards to sufficiently long times, post explosion, to do detailed nucleosynthesis calculations (an issue for which improvement is sought in project M04). As such, the present state of the art models must instead rely on parametric, or spherically symmetric, neutrino wind calculations to estimate the nucleosynthetic output of CCSNe. At present, these models suggest CCSNe are a less favourable site than binary neutron star mergers, but the neutrino microphysics within these models suffer from uncertainties which affect their nucleosynthesis predictions. A finding on Earth of 244Pu coincident in time, at 2 Myr ago, with previously discovered supernova-produced 60Fe would demonstrate that the r-process does occur in CCSNe, answering the outstanding question for the site of the r-process, while simultaneously providing immediate empirical insight to our understanding of the role of neutrinos in r-process nucleosynthesis.

快速中子俘获过程（英语：Rapid neutron capture process，简称r过程）是宇宙中至少一半丰度大于铁的元素产生的机制。它的位置仍然未知，确定它发生在哪里是核天体物理学中最突出的问题之一。目前理论上的候选地点是核心坍缩超新星（CCSNe）和双中子星星合并。目前最先进的3D超新星模型在计算上过于昂贵，无法在爆炸后足够长的时间内向外计算，以进行详细的核合成计算（项目M04中寻求改进的问题）。因此，目前最先进的模型必须依赖于参数或球对称中微子风计算来估计CCSNe的核合成输出。目前，这些模型建议CCSNe是一个不太有利的网站比双中子星星合并，但这些模型中的中微子微观物理遭受的不确定性，影响他们的核合成预测。在200万年前，在地球上发现的244 Pu与先前发现的超新星产生的60 Fe在时间上重合，这将证明r过程确实发生在CCSNe中，回答了r过程位置的悬而未决的问题，同时为我们理解中微子在r过程核合成中的作用提供了直接的经验见解。