Spectroscopic Investigations of Massive Binaries

大型双星的光谱研究

• 批准号: 0205297
• 负责人: Douglas Gies
• 金额: $ 25.74万
• 依托单位: Georgia State University Research Foundation, Inc.
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2002
• 资助国家: 美国
• 起止时间: 2002-08-01 至 2006-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0205297&HistoricalAwards=false
• 关键词: Spectroscopic; Investigations; Massive; Binaries

AST-0205297PI GiesThe majority of the most massive stars are born in close pairs that are destined to interact over their lifetime. The influence of a companion can dramatically alter the evolutionary paths of the stars: the mass donors can be stripped down to a fraction of their original size while the mass gainers can become rejuvenated as more massive and luminous stars. These altered stars will eventually explode as peculiar supernovae, and their remnants dominate the appearance of the high energy universe (as massive X-ray binaries containing neutron stars and black holes). Although the starting and end-points of binary evolution are understood the processes that forge the intermediate stages are still mysterious, and great uncertainties surround the issues of mass and angular momentum transfer and loss. This project will be an investigation of these processes at various stages in the evolutionary drama through spectroscopic studies of a number of key systems. The first part is a survey of two dozen targets for new binaries with hard to detect companions. The second section is an orbital analysis of the H a emission flux formed in the circumstellar gas in two currently interacting systems. The third part examines the link between mass transfer and the spin up of rapidly rotating stars, and includes a hunt for faint post-mass transfer companions of Be stars. The final component is a joint H a -X-ray study of mass transfer in massive X-ray binaries as documented in extensive H a spectroscopy obtained with the KPNO Coude Feed Telescope.***

AST-0205297PI Giesthe大多数最大的恒星都是近距离诞生的，注定会在他们的一生中相互作用。伴侣的影响可以极大地改变恒星的进化路径：可以将大量捐赠者剥离到其原始大小的一小部分，而质量增益者可以随着更大和发光的恒星的更新。这些改变的恒星最终将以奇特的超新星爆炸，它们的残余物占据了高能宇宙的外观（作为含有中子星和黑洞的巨大X射线二进制物）。尽管二进制进化的起点和终点已被理解为锻造中间阶段的过程仍然是神秘的，而且极大的不确定性围绕着质量和角动量转移和损失的问题。 该项目将通过对许多关键系统的光谱研究进行进化戏剧的各个阶段对这些过程的调查。第一部分是针对难以检测伴侣的新二进制文件的两打目标的调查。第二部分是对两个当前相互作用系统中偶性气体形成的h发射通量的轨道分析。第三部分研究了传质和快速旋转恒星的旋转之间的联系，并包括寻找微弱的质量后转移伴侣的恒星。最终部分是在大量X射线二进制物中进行的h-x射线研究，如用kpno coude feed望远镜获得的广泛h光谱。***