Three Dimensional Modeling of Core-Collapse Supernovae

核心塌缩超新星戏剧性地宣告了大质量恒星的死亡以及中子星、脉冲星和黑洞的诞生。它们是自然界中大多数重元素产生的地方。被视为核物理实验室的核心塌缩超新星产生了宇宙中密度和能量最高的一些超新星，在这个激烈的过程中，核物理、湍流流体力学、辐射传输和中微子物理的组合决定了恒星是否以及如何爆炸。然而，到目前为止，关于爆炸的确切机制的谜团还没有解开。该团队的一个论点是，过去几十年取得进展的一个根本障碍可能是缺乏适当模拟坍塌现象的代码、计算机和资源。这可以解释自上世纪60年代以来，S在展示爆炸的强大机制方面进展缓慢，令人痛苦的原因。然而，有了这个团队最近开发的最先进的计算机代码，现在可能是时候对天体物理学的这个核心问题进行最后的攻击了。深入研究三维中微子辐射流体力学，并运用最好的中微子和核物理，可能是演示和理解核塌缩超新星一般爆炸机制的关键。由于这些超新星模拟很容易为公众和学校提供支持，该团队计划制作视频产品用于公共演讲和网络传播。核塌缩超新星探索超核密度、高温和同位旋极端情况下物质的核和粒子物理。该项目通过探索天体物理爆炸中的核合成、中微子的性质和核物质的状态方程来支持国家科学院的实验核物理计划。数值模拟直接与FRIB和FIRE的低能程序、RHIC和LHC的高能实验以及JPARC、GSI、JLAB和NICA的超子-超子和超子-核子程序相连接。此外，核心塌缩超新星问题的解决将有利于美国和世界各地的观察者和仪器设计者正在进行的努力，他们从事的项目是确定元素的起源，测量引力波(LIGO)，并根据恒星核合成解释实验室核反应速率测量。

Core-collapse supernovae dramatically announce the death of massive starsand the birth of neutron stars, pulsars, and black holes. They are thesites where most of the heavy elements of Nature are created. Viewed as anuclear physics laboratory, core-collapse supernovae produce some of thehighest densities and energies in the Universe, and during this violentprocess a combination of nuclear physics, turbulent hydrodynamics,radiation transport, and neutrino physics determines whether and how thestar explodes. However, to date the puzzle of the precise mechanism ofexplosion has not been cracked. A thesis of this team is that afundamental impediment to progress over the last few decades may have beenthe lack of access to codes, computers, and resources with which toproperly simulate the collapse phenomenon. This could explain theagonizingly slow march since the 1960's towards demonstrating a robustmechanism of explosion. However, with the state-of-the-art computer codethis team has recently developed, the time may now be ripe to make a finalassault on this central problem in astrophysics. Going to fullythree-dimensional neutrino radiation-hydrodynamics and employing the bestneutrino and nuclear physics may together be the keys to demonstrating andunderstanding the generic core-collapse supernova explosion mechanism.Since these supernova simulations lend themselves easily to public andschool outreach, the team plans to generate video products for publictalks and web-based distribution.Core-collapse supernovae probe the nuclear and particle physics of matterat super-nuclear density, high temperature, and at extremes of isospin.This project supports the experimental nuclear physics program of the NSFby exploring nucleosynthesis in astrophysical explosions, the propertiesof the neutrino, and the equation of state of nuclear matter. The numerical simulations connect directly with the lower-energy programs ofFRIB and FAIR, the high-energy experiments carried out at RHIC and theLHC, and the hyperon-hyperon and hyperon-nucleon programs of JPARC, GSI,JLAB, and NICA. In addition, a solution to the core-collapse supernovaproblem will benefit ongoing efforts of observers and instrumentdesigners in the U.S. and around the world engaged in projects todetermine the origin of the elements, measure gravitational waves (LIGO),and interpret laboratory nuclear reaction rate measurements in light ofstellar nucleosynthesis.