Supernovae and Neutron Star Formation

超新星和中子星形成

• 批准号: 8914346
• 负责人: Adam Burrows
• 金额: $ 11.8万
• 依托单位: University of Arizona
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 1989
• 资助国家: 美国
• 起止时间: 1989-12-15 至 1993-11-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=8914346&HistoricalAwards=false
• 关键词: Supernovae; Neutron; Star; Formation

Even though theoreticians agree that supernova explosions derive their energy from the collapse of the progenitor star's core, they have found it very difficult to confirm this theory numerically. Recently, J. Wilson has succeeded in modelling SN ejection by the "delayed supernova explosion mechanism." According to this mechanism, energy from the progenitor star's core collapse is transferred to the envelope by neutrinos in a delayed fashion. The Principal Investigator (PI) proposes to investigate the viability and necessary conditions of Wilson's mechanism. The PI will use a one-dimensional relativistic hydrodynamic computer code, originally developed by Myra et al. The PI's specific focus will be on how the explosion, the resulting neutron star, and the neutrino emission spectrum are dependent upon the progenitor star's mass and structure. Furthermore, he will calculate theoretical neutrino burst signatures, simulate the star's mantle convection two- dimensionally, and investigate the evolution of X-ray and gamma- ray emissions. The 2-D code has been developed, debugged, and tested by Fryxell. As a final topic, unrelated to SN, the PI proposes to continue with his evolutionary calculations of brown dwarfs and very low mass stars.

尽管理论家们一致认为超新星爆炸的能量来自于前身恒星核心的坍塌，但他们发现很难从数字上证实这一理论。最近，J·威尔逊成功地用“延迟超新星爆炸机制”模拟了SN的抛射。根据这一机制，前驱恒星核心坍塌产生的能量被中微子以延迟的方式转移到包层。首席调查员(PI)建议调查威尔逊机制的可行性和必要条件。PI将使用一维相对论流体力学计算机代码，该代码最初由Myra等人开发。PI的具体焦点将是爆炸、由此产生的中子星和中微子发射光谱如何依赖于前驱恒星的质量和结构。此外，他将计算理论上的中微子爆发特征，二维模拟恒星的地幔对流，并研究X射线和伽马射线发射的演变。2-D代码已经由Fryxell开发、调试和测试。作为与SN无关的最后一个话题，PI建议继续他对褐矮星和极低质量恒星的进化计算。