Theoretical Investigations of the Equation of State for Stellar Interiors

PI建议为恒星内部计算开发一个统一的状态方程。这些模型是恒星天文学的基础，它们为理解正常恒星的结构提供了基础，也为恒星演化的后期阶段提供了模型。该项目的主要目标是调和目前存在于确定太阳内部结构的两种相互竞争的方法之间的不一致性。pi将使用他们的内部模型和GONG太阳振荡数据之间的直接比较。至少在低密度区域，这将为导出的状态方程提供可靠的测试。这些结果可能有助于提高对太阳氦丰度的测定，这一数值对一般的恒星模型和氦的宇宙学起源都有重大影响。它们也有可能改进其他恒星演化阶段的模型计算，比如低密度的巨星到高密度的白矮星。本项目由美国国家科学基金会恒星天文学和天体物理学项目（AST/SAA）资助

AST-9987391Dappen, WernerThe PI proposes to develop a unified equation of state for stellar interior computations. Such models are the foundation of stellar astronomy, and they provide the basis for understanding the structure of normal stars, as well as models for later stages of stellar evolution. The main goal of the project is to reconcile inconsistencies that currently exist between two competing approaches to determining the interior structure of the Sun. The PIs will use direct comparisons between the their interior models and GONG solar oscillation data. This should provide firm tests of the derived the equation of state, at least in low density regions. The results may help improve the determination of the Sun's helium abundance, a value that has substantial impact on stellar models in general and on the cosmological origins of helium. They also have the potential to improve model calculations for other stellar evolutionary stages, such as low density giant stars to high density white dwarf stars.Funding for this project was provided by the NSF program for Stellar Astronomy & Astrophysics (AST/SAA).***