Supernovae and Astrophysical Gas Dynamics

超新星和天体物理气体动力学

• 批准号: 9016687
• 负责人: Roger Chevalier
• 金额: $ 14.1万
• 依托单位: University of Virginia Main Campus
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 1991
• 资助国家: 美国
• 起止时间: 1991-02-15 至 1994-10-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9016687&HistoricalAwards=false
• 关键词: Supernovae; Astrophysical; Gas; Dynamics

The supernova phase of evolution in massive stars is important to understand because it is during this violent stage that most of the heavy element atoms in the Universe are created, including the iron-group of elements responsible for life, and the generation of magnetic fields in planets. Supernova SN1987a is arguably the most intensively studied object outside the solar system since its explosion in the Large Magellanic Cloud was first observed in early 1987. Already studies of this object, the first bright supernova, in the modern era of astronomy, have uncovered several surprises, for example, that stars that become supernovae can be red in color rather than blue, as astronomical theories have predicted. Moreover, Supernova SN1987a, being one of only two supernovae to be studied continuously since its outburst, furnishes a unique opportunity to understand the very early evolution of a supernova, e.g., over the first decade. The Principal Investigator (PI) proposes to construct theoretical models to explain the emission of light from SN1987a using the most up-to-date information on shock wave physics. Although it is thought that the slowly fading light outputs of most supernovae are powered by the radioactive decay of unstable nickel and cobolt isotopes, several details of the light output in SN1987a rule out this possibility. The PI intends to focus on this problem in this program and to construct numerical models to that would include effects by the most likely alternative mechanisms: (1.) interaction of the exploding supernova gas shell with material lingering near the star that was previously part of a "stellar wind" ejected by unrelated causes, and (2.) the generation of a second shock wave caused by the birth of a magnetized neutron star (pulsar) as a consequence of the supernova explosion. The answer to this question is expected to affect our understanding of a significant fraction of supernova during their early phases, and will have a critical bearing on attempts to understand later stages of supernovae.

大质量恒星的超新星演化阶段对于 因为正是在这个暴力的阶段， 宇宙中的重元素原子被创造出来，包括 铁-负责生命的元素群，以及 行星的磁场 超新星SN 1987 a可以说是 太阳系外被深入研究的天体， 大麦哲伦星云中的爆炸首次被观测到是在1970年代早期。 1987. 对这颗第一颗明亮的超新星的研究， 在现代天文学中，发现了一些令人惊讶的现象， 例如，成为超新星的恒星可能是红色的 而不是天文学理论预测的蓝色 此外，超新星SN 1987 a是仅有的两颗超新星之一， 自其爆发以来一直被不断研究， 有机会了解超新星的早期演化， 例如，在一个实施例中，在第一个十年。 主要研究者（PI） 建议建立理论模型来解释排放 使用SN 1987 a的最新信息进行光分析 冲击波物理学 尽管人们认为大多数植物的缓慢衰落的光输出 超新星是由不稳定的镍的放射性衰变提供能量的 和钴同位素，SN 1987 a光输出的几个细节 排除这种可能性。 PI打算关注这个问题 在这个程序中，并建立数值模型，将 包括最可能的替代机制的影响： （1.） 超新星爆炸气体壳层与物质的相互作用 在这颗星星附近徘徊，这颗恒星以前是“恒星”的一部分， “风”由不相关的原因喷出，和（2）。的生成 由磁化中子星星诞生引起的第二次冲击波 （脉冲星）是超新星爆炸的结果。 答案 这一问题的答案将影响我们对 在超新星早期阶段， 将对理解后期阶段的尝试产生重要影响 关于超新星