AN OBSERVATIONAL STUDY OF CENTRAL STARS OF PLANETARY NEBULAE

行星状星云中心恒星的观测研究

基本信息

批准号：
63540189
负责人：
YAMASAKI Atsuma
金额：
$ 1.73万
依托单位：
UNIVERSITY OF TOKYO
依托单位国家：
日本
项目类别：
Grant-in-Aid for General Scientific Research (C)
财政年份：
1988
资助国家：
日本
起止时间：
1988 至 1989
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-63540189/
关键词：
Central stars of planetary nebulae Close binary systems Reflection effect Solar-type chromospheric active stars Triple system Optical observation 分光観測測光観測

项目摘要

We made optical observations of close binary central stars of planetary nebulae in order to obtain reliable physical quantities of central stars. Relating to the evolution of main- sequence close binaries toward binary central stars of planetary nebulae, we also studied close binaries on or near the main sequence.Among central stars of planetary nebulae, we made optical spectroscopic and photometric observations of three close binary central stars, LT-5, HFG1, and UU Sge, using the 188-cm and 91-cm telescopes at Okayama and Dodaira Observatories of National Astronomical Observatory of Japan (NAOJ). We also analyzed data taken at Mauna Kea Observatory using University of Hawaii 224-cm and 61-cm telescopes (supported by the Grants-in-Aid for Overseas Scientific Research [Head Investigators: Prof. T. Kogure (1988) and Prof. T. Tsuji (1989)] of the Ministry of Education, Science, and Culture).LT-5: it was found that (a) the G-star rotates with a period of 1.200 days; (b) the G-star and its close companion form an inner system with the orbital period of 1.755 days; (c) the existence of a third body (a hot star which excites the nebula) is deduced from the change of systemic velocities with a period of - 2000 days (an outer system). Physical quantities of the component stars are discussed. H. L. Malasan, graduate student, analyzed the data and presented MSc Thesis.HFG1: we obtained an almost complete light curve, confirming the discovery by Grauer et al. We interpreted the variation of light by the reflection effect and obtained a preliminary model for the binary central star system.UU Sge: we obtained for the first time a radial velocity curve, and discussed physical quantities of the system.We analyzed three main-sequence/post-main-sequence binaries, delta Cap, UZ Pup, and DD Mon; deduced physical quantities of components; and discussed briefly their binary evolution.

我们对行星状星云的近距离双星中心恒星进行了光学观测，以获得可靠的中心恒星物理量。关于主序邻近双星向行星状星云双星中心恒星的演化，我们还研究了主序带上或附近的邻近双星。在行星状星云中心恒星中，我们对三颗邻近双星中心恒星进行了光学光谱和光度观测、LT-5、HFG1 和 UU Sge，使用国家天文台冈山和堂平天文台的 188 厘米和 91 厘米望远镜日本（NAOJ）。我们还分析了使用夏威夷大学 224 厘米和 61 厘米望远镜在莫纳克亚天文台获取的数据（由海外科学研究补助金支持[首席研究员：T. Kogure 教授（1988 年）和 T 教授） .Tsuji (1989)] 文部科学省).LT-5: 发现 (a) G 星的自转周期为1.200 天； (b) G星与其近伴星形成一个轨道周期为1.755天的内系统； (c) 第三天体（激发星云的热星）的存在是根据系统速度在 - 2000 天的周期内的变化（外部系统）推断出来的。讨论了组成恒星的物理量。研究生 H. L. Malasan 分析了数据并提交了硕士学位论文。HFG1：我们获得了几乎完整的光变曲线，证实了 Grauer 等人的发现。我们通过反射效应解释了光的变化，得到了双中心星系统的初步模型。UU Sge：我们首次得到了视向速度曲线，并讨论了系统的物理量。我们分析了三个主序/后主序双星、delta Cap、UZ Pup 和 DD Mon；推导出元件的物理量；并简要讨论了它们的二元演化。