Impact of Stellar structure on Core-collapse Supernovae and their Ejecta

恒星结构对核心塌陷超新星及其喷射物的影响

• 批准号: 1713750
• 负责人: Eric Lentz
• 金额: $ 1.51万
• 依托单位: University of Tennessee Knoxville
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2017
• 资助国家: 美国
• 起止时间: 2017-09-01 至 2019-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1713750&HistoricalAwards=false
• 关键词: Impact; Stellar; structure; Core; collapse

Core-collapse supernovae (CCSN) are direct probes of stellar evolution and the dominant producers of heavy elements. Significant advancement in our understanding of the CCSN mechanism has occurred in the last decade, highlighted by the understanding that the CCSN problem involves the complex interaction of many physical inputs that can only be fully considered in three-dimensional (3D) simulations. The number of 3D simulations, which include sufficient realistic physics, that have been completed is still small and the simulations are generally under-resolved. Recent observational surveys have greatly increased the number of well observed CCSN and identified many of the pre-supernova stars, establishing a more direct relationship between the characteristics and the details of the explosion.This project will survey the range of the stellar mass of CCSN progenitors using the state-of-the-art CCSN code Chimera on the Blue Waters system to understand how the variations in pre-supernova structure affect the explosive outcomes. The simulations will begin from progenitor stars that span the range of stellar masses from the lightest to heaviest stars that might explode. The progenitor star models will be from the first generation of stars formed from the primordial gas of the Big Bang as there exists a class of second-generation stars contaminated by only the ejecta of first-generation supernovae that offer a unique opportunity to measure the ejected products of individual CCSN. This choice offers an important contrast to prior studies which have focused on metal-rich stars. The project will compute five 3D simulations over the course of 2 years with 1-degree resolution. This surpasses the resolution of any current self-consistent, full-physics CCSN simulation.The broader impacts of the project include the engagement of local and visiting students (graduate and undergraduate) and post-docs, providing training in both astrophysics and high-performance computing that our students and post-docs carry with them to later jobs in academia and industry. The project will also make frequent public lectures on supernova-related topics to enhance public understanding.

核心塌陷超新星（CCSN）是恒星演化的直接探测器，也是重元素的主要产生者。过去十年，我们对 CCSN 机制的理解取得了重大进展，尤其是我们认识到 CCSN 问题涉及许多物理输入的复杂相互作用，而这些物理输入只能在三维 (3D) 模拟中充分考虑。已完成的包含足够真实物理的 3D 模拟数量仍然很少，而且模拟的解析度普遍较低。最近的观测调查大大增加了观测良好的 CCSN 数量，并识别了许多超新星前恒星，在特征和爆炸细节之间建立了更直接的关系。该项目将使用 Blue Waters 系统上最先进的 CCSN 代码 Chimera 来调查 CCSN 前身恒星质量的范围，以了解超新星前结构的变化如何影响 爆炸性的结果。模拟将从祖星开始，这些祖星的恒星质量范围从最轻到最重的可能爆炸的恒星。祖星模型将来自由大爆炸的原始气体形成的第一代恒星，因为存在一类仅被第一代超新星喷射物污染的第二代恒星，这为测量单个CCSN的喷射物提供了独特的机会。这一选择与之前关注富金属恒星的研究形成了重要对比。该项目将在 2 年内以 1 度分辨率计算 5 次 3D 模拟。这超越了当前任何自洽、全物理 CCSN 模拟的分辨率。该项目的更广泛影响包括本地和访问学生（研究生和本科生）和博士后的参与，提供天体物理学和高性能计算方面的培训，我们的学生和博士后将这些培训带到学术界和工业界的后续工作中。 该项目还将经常就超新星相关话题进行公开讲座，以增进公众的了解。