Stellar Spectroscopy and Nucleosynthesis

恒星丰度的测定是从它们的高 分辨率光谱构成了最基本的观测基础 了解恒星在其生命周期中是如何演化的。 的 主要研究者（PI）将继续他以前的NSF- 支持的工作，以确定内部核武器 反应是重元素产生的原因， 随后改变了星际气体的化学成分 通过恒星质量损失影响未来的演化 一代又一代的明星 PI的新工作将侧重于 我们银河系和银河系中恒星的化学成分 南半球的麦哲伦云。 除了 专注于生产某些重元素（Ge，Rb， 和Mo），PI将集中在13 C，轻金属丰度 在大质量恒星中，锂丰度在太阳型恒星中， 在已知的化学性质特殊的A星中存在明显的化学异常 “牧夫座λ”恒星 除了澄清 恒星核心的重元素核反应网络， 研究有望帮助我们理解 包层中对流混合和辐射扩散的作用 在“主序星”上的许多恒星。"

The determination of the abundances of stars from their high resolution spectra forms the most fundamental observational basis for understanding how stars evolve through their life cycles. The Principal Investigator (PI) will continue his previous NSF- supported work to determine to what extent interior nuclear reactions are responsible for the creation of heavy elements, which subsequently alter the chemical composition of interstellar gas via stellar mass loss and influence the evolution of future generations of stars. The PI's new work will focus both on the chemical composition of stars in our own Galaxy and in those of the Magellanic Clouds in the Southern hemisphere. In addition to concentrating on the production of certain heavy elements (Ge, Rb, and Mo), the PI will concentrate on 13C, the light-metals abundances in massive stars, Li abundance in solar-type stars, and the apparent chemical anomalies in chemically peculiar A stars known as "lambda Bootis" stars. In addition to clarifying the role of networks of heavy-element nuclear reactions in stellar cores, this research is expected to help our understanding of the possible roles of convective mixing and radiative diffusion in the envelopes of many stars on the "main sequence."