The Physical Properties of Hot and Cool Massive Stars as a Function of Metallicity in the Local Group

热和冷大质量恒星的物理性质作为本星系群金属丰度的函数

• 批准号: 0604569
• 负责人: Philip Massey
• 金额: --
• 依托单位: Lowell Observatory
• 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: 2006-08-01 至 2010-01-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0604569&HistoricalAwards=false
• 关键词: Physical; Properties; Hot; Cool; Massive

This work here is motivated by the need for accurate physical properties of massive starsof varying metallicity in order to understand their evolution, star formation processes, andfeedback mechanisms into the interstellar medium. Of particular interest is temperature,which plays a key role in transforming observations (spectral type and photometry) intophysical properties (effective temperature, surface gravity, bolometric luminosity, radius,and inferred mass). In this project, an improvement of the effective temperature scales forboth hot (30,000 to 50,000K) main-sequence and cool (3,000 to 4000K) evolved (redsupergiant) massive stars will be undertaken This will be accomplished using high qualityoptical spectra (plus infrared photometry in the case of the cool giants) and the latestgeneration of stellar atmosphere models at both temperature extremes. Of particularimportance is that these calibrations will be developed as a function of metallicity andtherefore applicable to other studies of high mass stars throughout the local group.Undergraduate students will be involved in this work through the NSF sponsoredResearch Experiences for Undergraduates and MIT Field Camp programs. The studentswill be full collaborators and take part in data acquisition, analysis, writing, and thepresentation of results at scientific meetings. This research will also be featured in publictalks given through the Lowell Observatory visitor program and at other venues. The datacollected here will also be made public once accepted for publication.

这项工作的动机是为了了解不同金属丰度的大质量恒星的准确物理性质，以了解它们的演化，星星形成过程和反馈机制到星际介质。特别令人感兴趣的是温度，它在转换观测（光谱类型和光度学）到物理性质（有效温度，表面重力，辐射热光度，半径和推断质量）中起着关键作用。在这个项目中，将对热的（30，000至50，000 K）主序星和冷的（3，000至4000 K）演化（红超巨星）大质量恒星的有效温标进行改进。这将使用高质量的光谱（在冷巨星的情况下加上红外测光）和最新一代的恒星大气模型在两个极端温度下完成。特别重要的是，这些校准将作为金属丰度的函数来开发，因此适用于整个本地组的其他高质量恒星的研究。本科生将通过NSF资助的本科生研究经验和麻省理工学院野外营地计划参与这项工作。学生将是完全合作者，并参与数据采集，分析，写作和在科学会议上展示结果。这项研究也将在洛厄尔天文台游客计划和其他场所举行的公共演讲中展出。这里收集的信息一旦被接受出版，也将被公开。