Abundance of the Elements and Stellar Chemistry

研究人员将为解释恒星环境中气体和尘埃的丰度和化学成分提供一个基本框架。这些研究对天体物理学和宇宙化学的许多不同领域都很重要。 一项主要任务是对我们太阳系元素丰度的参考集进行大规模更新，这些参考集来自陨石样本;这些所谓的“太阳丰度”被用作研究宇宙中其他恒星和星系性质的基本参考。研究人员将领导一项跨校园倡议，鼓励计算机科学专业的本科生参与这项研究。这项研究的结果被纳入新的/修订的教科书和课堂材料和讲座。这位女研究员为考虑从事科学工作的年轻妇女树立了榜样。外联：调查人员与大学公共事务办公室合作，发布新闻稿，向公众传播调查结果;例如，关于褐矮星的天气，在一个熔岩行星上下卵石雨，或者关于蒸发地球。他们的研究也支持博士论文和本科生研究。元素丰度是天文学中许多化学模型的重要输入。太阳元素丰度通常被用作描述天体的参考。建议的化学计算是相关的理解气体分子和凝析油形成的原恒星盘（有和没有行星形成），并在喷出物的演化恒星的饲料灰尘和气体的ISM，从新的恒星和行星系统的起源。垂死的恒星很少有太阳的整体组成，特别是不包括C，N和O，它们决定了氧化还原条件。气体和尘埃的化学性质强烈依赖于C/O比，这项研究的目的是推导出一套完整的非太阳条件下所有元素的冷凝温度。在非太阳金属丰度的化学工作是高度相关的行星形成模型周围的高金属丰度的恒星，以及冷凝周围的低金属丰度的恒星，甚至在高红移的尘埃星系。

The investigators will provide a fundamental framework for interpreting the abundances and chemical composition of the gas and dust in stellar environments. The investigations are important for many different areas in astrophysics and the chemistry of the cosmos. A major task is a large update to the reference set of abundances of the elements in our own Solar System, derived from samples of meteorites; these so-called "solar abundances" are used as a fundamental references for the study of properties of other stars and galaxies in the universe.The investigators will lead a cross-campus initiative, encouraging undergraduate students from the computer sciences to participate in this research. The results from this research are integrated into new/revised textbooks and in class materials and lectures. The female investigator serves as a role model for young women considering scientific careers. Outreach: The investigators work with the university public affairs office to issue press releases to spread results to the public; e.g., about brown dwarf weather, raining pebbles on a molten-rock planet, or about evaporating the Earth. Their investigation also supports a PhD thesis and undergraduate research.Element abundances are an important input to many chemical models in astronomy. The solar elemental abundances are commonly used as a reference when describing astronomical objects. The proposed chemistry calculations are relevant for understanding gas molecule and condensate formation in protostellar disks (with and without planetary formation); and in ejecta of evolved stars that feed dust and gas to the ISM, from which new stellar and planetary systems originate. Dying stars rarely have overall solar composition, especially not for C, N, and O, that govern redox conditions. The gas and dust chemistry strongly depends on the C/O ratio and the study aims to derive a complete set of condensation temperatures for all elements under non-solar conditions. The proposed work for chemistry at non-solar metallicities is highly relevant to planet formation models around high metallicity stars, as well as condensation around low-metallicity stars or even in dusty galaxies at high red-shift.