RUI: Time-Resolved Observations of Classical and Dwarf Novae

RUI：经典和矮新星的时间分辨观测

• 批准号: 9115131
• 负责人: Allen Shafter
• 金额: $ 10.05万
• 依托单位: San Diego State University Foundation
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 1992
• 资助国家: 美国
• 起止时间: 1992-02-01 至 1994-07-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9115131&HistoricalAwards=false
• 关键词: RUI; Time; Resolved; Observations; Classical

Novae, dwarf novae, novae-like stars are all thought to be pairs of stars in which a "main sequence" star is slowly expanding and transferring some of its matter onto an orbiting "white dwarf." The heating of fresh hydrogen from the first star results in thermonuclear reactions on the white dwarf's surface, leading to a vast class of rapid brightenings we observe as nova-type stars. Many astronomers are trying to understand whether each of these systems is the same type of object in a different stage of evolution or whether they are fundamentally different types of objects. In this two-year study the Principal Investigator (PI) and a student will monitor a dozen binary stars that have under- gone nova eruptions in the past to examine the periods and other orbital characteristics that would lead to improved estimates of these stars' masses and radii. This is expected to double the number of stars for which these fundamental parameters are known and to permit a better estimate to be made of the distribution of their periods. The PI anticipates that this study will contribute to resolving whether nova undergo rapid mass transfer events followed by little exchanges between the two stars over longer times. A resolution of this issue will help determine whether novae, dwarf novae, and nova-like systems are the same system merely observed in different stages of evolution. This is an award under the auspices of the NSF's Research for Undergraduate Institutions program and is expected to contribute to the scientific instruction of graduate and undergraduate students at the PI's institution.

新星，矮新星，类新星恒星都被认为是成对的 其中一颗“主序星”星星正在缓慢膨胀， 将部分物质转移到轨道上的“白色矮星”上。" 来自第一颗星星的新鲜氢被加热， 白色矮星表面的热核反应， 我们观测到的一大批快速增亮的新星 星 许多天文学家试图了解 这些系统是同一类型的对象在不同的阶段， 或者它们是否是根本不同类型的 对象 在这项为期两年的研究中，主要研究者（PI） 一个学生将监测十几个双星， 去新星爆发在过去检查的时期和其他 轨道特性，将导致改进的估计 这些恒星的质量和半径 预计这一数字将翻一番 这些基本参数的恒星数量 已知的，并允许更好地估计， 它们的周期分布。 PI预计， 研究将有助于解决新星是否经历快速 质量转移事件，随后是 两颗星在更长的时间。 这个问题的解决将 帮助确定新星、矮新星和类新星系统 是同一个系统，只是在不同的阶段观察， 进化 这是美国国家科学基金会赞助的一个奖项 研究本科院校计划，并预计 为研究生的科学指导做出贡献， PI所在机构的本科生。