Numerical Study of Stellar Collapse Neutron Star Collision, Heavy Ion Collisions

威尔逊博士的研究目标分为三个 主要类别：超新星、重离子碰撞和中子 星星碰撞。 超新星的研究包括澄清 超新星爆炸机制的性质，利用数值 计算机模型，调查粒子物理学的影响， 超新星事件和提供理论和设计支持 一个超新星中微子观测站的原型 构建了 从所有这些预期有趣的结果 项目，特别是对大质量中微子模型的限制 (with它们的相关振荡性质）和轴子质量 限制. 重离子碰撞项目的基础是模拟 重离子碰撞的流体动力学近似 重子和π介子的平均场模型。 通过比较 低能重离子碰撞实验模型 （大约每核子一个GeV）超新星的重要信息 将导出状态方程。在更高的碰撞能量下， 将处理核透明度问题。 研究中子星碰撞的数值程序 几乎已经完成。 频率和总能量 在引力辐射中发出的辐射将被计算， 在最后的螺旋向内运动中， 和中子星星对的合并。

Dr. Wilson's research objectives are divided into three major categories: supernovae, heavy ion collisions and neutron star collisions. Research in supernovae includes the clarification of the nature of the supernova explosion mechanism utilizing a numerical computer model, surveying the implications to particle physics of supernova events and providing theoretical and design support for a prototype supernovae neutrino observatory now being constructed. Interesting results are expected from all these projects, in particular, restraints on massive neutrino models (with their associated oscillation properties) and axion mass limits. The heavy ion collision project is based on modeling the collision of heavy ions by a hydrodynamical approximation for the baryons and a mean field model for the pions. From comparison of the model with heavy ion collision experiments at low energies (about one GeV per nucleon) important information for supernovae equations of state will be derived. At higher collision energies, the issue of nuclear transparency will be addressed. A numerical program to study the collisions of neutron stars has almost been completed. The frequency and total energy emitted in gravitational radiation will be computed as well as the neutrino signal expected during the final spiraling inward and coalescence of a neutron star pair.