Collaborative Research: Dust formation around carbon stars: astromineralogy and the condensation sequence

合作研究：碳星周围尘埃的形成：天文学和凝结序列

• 批准号: 0607341
• 负责人: Angela Speck
• 金额: $ 19.45万
• 依托单位: University of Missouri-Columbia
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2006
• 资助国家: 美国
• 起止时间: 2006-07-15 至 2010-06-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0607341&HistoricalAwards=false
• 关键词: Collaborative; Research; Dust; formation; around

This research is motivated by the need to better understand the role of dust inastrophysical environments. Dust is a vital ingredient in the star formation process aswell as in planet forming disks. It is a source of mass loss from evolved stars (throughradiation pressure on dust grains) and intimately links the radiation field to thecircumstellar material. Dust also contributes to several aspects of interstellar processessuch as gas heating and the formation of molecules. The work to be undertaken here is specifically centered on characterizing the precise nature of dust grains around cool carbon stars as these are the source of the bulk of the Galaxy's carbon-rich dust. Byknowing the initial state of the dust from such stars, the effects of the dust in theinterstellar medium can be more accurately quantified. Moreover, the relatively benignenvironment surrounding such stars simplifies the chemistry, which in turn facilitates theunderstanding of the various processes in operation. The properties of the grains are alsotied to the evolution of the star itself, thus the precise nature of the dust must be assessedin order to understand this evolution. Finally, recent Spitzer Space Telescopeobservations of carbon stars in the Magellanic Clouds suggest a different dustcondensation sequence compared to Galactic carbon stars which may well permit theeffects of metallicity on dust formation to be investigated.The tools to be applied here include infrared spectroscopy and imaging, radiative transfermodeling, laboratory spectroscopy, and archival data mining. They will be used to testcurrent theories of dust formation in carbon star environments and how thesecondensation sequences are effected by the initial mass and metallicity of the parent stars.Furthermore, the imaging and radiative transfer studies should provide insight into thecauses of axisymmetric structures seen in planetary and protoplanetary nebulae.This project includes the participation and training of a doctoral student who will be anintegral part of the research program. The student will be expected to present results atboth conferences and public talks thereby combining training with public outreach.

这项研究的动机是需要更好地了解尘埃在天体物理环境中的作用。尘埃是星星形成过程和行星形成盘的重要成分。它是演化恒星质量损失的来源（通过尘埃颗粒上的辐射压力），并将辐射场与恒星物质密切联系起来。尘埃也有助于星际过程的几个方面，如气体加热和分子的形成。这里要进行的工作特别集中在表征冷碳星周围尘埃颗粒的精确性质，因为这些是银河系大部分富碳尘埃的来源。通过了解这些恒星尘埃的初始状态，可以更准确地量化星际介质中尘埃的影响。此外，这些恒星周围相对温和的环境简化了化学过程，这反过来又有助于理解各种运行过程。尘埃颗粒的性质也与星星本身的演化有关，因此，为了理解这种演化，必须评估尘埃的精确性质。最后，斯皮策太空望远镜最近对麦哲伦星云中碳星的观测表明，与银河系碳星相比，它有一个不同的尘埃凝结序列，这很可能使我们能够研究金属丰度对尘埃形成的影响。在这里应用的工具包括红外光谱和成像、辐射传输模型、实验室光谱和档案数据挖掘。它们将被用来检验碳星星环境中尘埃形成的现有理论，以及这些凝结序列如何受到母星初始质量和金属丰度的影响。成像和辐射传输研究应能深入了解行星状星云和原行星状星云中轴对称结构的成因。该项目包括一名博士生的参与和培训，该博士生将成为该项目的一个组成部分。研究计划。学生将被要求在会议和公开演讲中展示成果，从而将培训与公共宣传相结合。