Stellar Spectroscopy and Nucleosynthesis

随着时间的推移，由于恒星的质量损失(如超新星和新星爆炸、恒星风)导致重元素的浓缩，星系的化学成分发生了变化。恒星通过其内部的核反应产生重元素。因此，恒星的演化和它们所在的星系的演化是密切相关的。首席研究人员(PI)提出了一项利用定量光谱学来确定银河系恒星大气化学成分的计划。他们的基本目标是解决有关银河系的化学演化、特殊的主序恒星、红巨星及其核反应等悬而未决的问题。拟议的计划是过去由NSF支持的工作的延续。

In the course of time, the chemical compositions of galaxies change due to heavy element enrichment by mass loss from stars (e.g., supernova and nova explosions, stellar winds). The stars produce the heavy elements by nuclear reactions in their interiors. Thus, the evolution of stars and that of the galaxies within which they reside are intimately connected. The Principal Investigators (PIs) propose a program of determining the chemical composition of the atmospheres of stars in our Galaxy using quantitative spectroscopy. Their fundamental aim is to address unresolved issues concerning the chemical evolution of the Galaxy, peculiar main sequence stars, and red giants and their nuclear reactions. The proposed program is a continuation of past work supported by NSF.