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

威尔逊博士的研究目标分为三大类：超新星、重离子碰撞和中子星碰撞。超新星的研究包括利用数值计算机模型澄清超新星爆炸机制的性质，调查超新星事件对粒子物理的影响，并为正在建设的原型超新星中微子天文台提供理论和设计支持。所有这些项目都有望得到有趣的结果，特别是对大质量中微子模型（及其相关振荡特性）和轴子质量极限的限制。重离子碰撞项目的基础是用重子的流体动力学近似和介子的平均场模型来模拟重离子的碰撞。通过与低能重离子碰撞实验（每核子约1 GeV）的比较，将得到超新星状态方程的重要信息。在更高的碰撞能量下，核透明度问题将得到解决。一个研究中子星碰撞的数值程序已基本完成。将计算引力辐射发射的频率和总能量，以及中子星对最终向内旋转和合并过程中预期的中微子信号。

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.