Collaborative Research: The Young Remnants of Massive Star Supernovae

建议ID：AST-0307366/AST-0307256机构：弗吉尼亚大学/北卡罗来纳州立大学PI：Chvalier，Roger/Blondin，JohnDr.弗吉尼亚大学的罗杰·切瓦利埃和北卡罗来纳州立大学的约翰·布朗丁博士获得了对大质量恒星超新星年轻残骸进行建模的资金。在它们的一生中，大质量恒星在不同的演化阶段经历了质量损失。当它们最终以超新星的形式结束生命时，相互作用既取决于导致爆炸的质量损失过程，也取决于爆炸恒星的结构。这种相互作用的多波长观测将被模拟为各种类型的大质量恒星超新星。真实的恒星模型将被用于相互作用的流体力学模型中，包括星周材料中不均匀结构的影响。将要研究的物理过程包括：X射线辐射的产生；快速冲击波中的电子加热；相对论电子的产生和演化及其发射；密集相互作用壳中可能形成的尘埃；碰撞加热尘埃的红外发射；以及预期各种相互作用成分的光谱性质。各种大质量恒星超新星的质量损失特性将被确定，并与演化模型的预期有关。这项工作对天体物理学具有广泛的影响，因为它与大质量恒星的晚期演化、重元素返回星际介质以及高能量密度下的物理过程有关。这项研究将在弗吉尼亚大学、北卡罗来纳州立大学和斯德哥尔摩天文台之间建立联系。这项工作还将对一名研究生进行计算机模拟技术方面的培训。描述三维模拟结果的模块将被添加到一个已经提供现有代码的公共网站。最后，研究成果将整合到本科课程和公开讲座中。

Proposal ID: AST-0307366 / AST-0307256Institution: University of Virginia / North Carolina State UniversityPI: Chevalier, Roger / Blondin, JohnDr. Roger Chevalier at the University of Virginia and Dr. John Blondin at North Carolina State University are awarded funds to model the young remnants of massive star supernovae. During their lifetimes, massive stars undergo mass loss during various evolutionary phases. When they finally end their lives as supernovae, the interaction depends on both the mass loss processes leading up to the explosion and the structure of the exploding star. Multi-wavelength observations of this interaction will be modeled for various types of massive star supernovae. Realistic stellar models will be used in hydrodynamic models of the interaction, including the effects of inhomogeneous structure in the circumstellar material. The physical processes to be investigated include the production of X-ray emission, electron heating in fast shock waves, the production and evolution of relativistic electrons and their emission, possible dust formation in a dense interaction shell, infrared emission from collisionally heated dust, and spectral properties expected for various interaction components. The mass loss properties of various kinds of massive star supernovae will be determined and related to expectations from evolutionary models. This work has broad implications for astrophysics in that it is relevant to the late evolution of massive stars, the return of heavy elements to the interstellar medium, and physical processes at high energy densities. The research will build ties between the University of Virginia, North Carolina State University, and Stockholm Observatory. This work will also result in the training of a graduate student in computer simulation techniques. A module describing the results of three-dimensional simulations will be added to a public web site that already offers the existing code. Finally, the research results will be integrated into undergraduate courses and public lectures.