| 题名 | 密近双星的演化链 |
| 作者 | 李立芳 |
| 学位类别 | 硕士 |
| 答辩日期 | 1998 |
| 授予单位 | 中国科学院云南天文台 |
| 授予地点 | 昆明 |
| 导师 | 刘清耀 |
| 关键词 | 双星 浊化链 密近双星 |
| 中文摘要 | 本文对密近双星演化研究的历史和现状作了简要的回顾和概括。从观测和理论计算等不同角度讨论了判断密近双星演化阶段的主要方法。在大量观测资料的基础上得到了不同类型密近双星的性质和演化阶段。在总结前人工作的基础上，提出了密近双星演化链研究中有待进一步研究的问题。给出了短周期食双星AP Aur的B、V两色光电测资料。该双星的光变曲线是不对称的，第二极大明显比第一极大高，即具有明显的反O'Connell效应。用Wilson程序（92版）对实测光变曲线和实测数据进行分析，得到了该双星的轨道参量和物理参量。结果表明AP Aur是一个深相接的A次型W Uma型相接双星。根据AP Aur的性质，分析了产生O'Connell效应的物理机制。指出物质交流效应不能解释AP Aur光变曲线的不对称性。导致AP Aur光变曲线不对称的物理原因可能是子星的类太阳活动（或）公共包层中的环流效应。然后利用Wilson方法求出了AP Aur的星斑参量和轨道参量。最后讨论了AP Aur的演化阶段和它的演化前途，主要结论如下：1. AP Aur是一个已演化了的相接双星，这带有一个已演化离开主序的次子星。2. AP Aur是一个相接程度很高的相接双星，同时质量比很小，这样的双星系统是不稳定的。由于它的不稳定性，次星可能被主星“吞星”掉而演化成一个单星；或者通过公共包层演化，抛掉公共包层而演化成激变变星。 |
| 英文摘要 | In this thesis, We have made a recapitulation about the studies in the history and the current state of the close binary evolution. The methods judging the evolutionary stage of the close binary are discussed from the observational and theoretical angles. Based on the observatory data, the peoperties and the evolutionary stage of the different kinds of close binaries are obtained. And on the basis of the former authors' work, the difficulties in studying the evolutionary links are presented. photoelectric observations in B and V bands for short period eclipsing binary AP Aur are presented. The light-curve asymmetry with Max. II brighter than Max. I(called inverse O'Connell effect) is seen in both bands. The light curves have been analysed by using the 1992 version of Wilson-code, the orbital and physical parameters are obtained. The photo- metric solutin indicate that AP Aur is a deep-contact A-type W UMa bin-aries. According to the properties of the system AP Aur, the mechanisms causing the the O'Connell effect are discussed. The analysis indicate that the asymmetry of the light curve of AP Aur can not be caused by the mass transfer. The mechanisms causing the O'Connell effect in this system may be the sun-like activities or circulation effect. Then the spotted parameters and the orbital parameters are obtained by using Wilson-code. Finally, the present evolutioary stage and the evolutionary trends in the future of this system are discussed. Conclutions are following: 1. AP Aur is an evolved binary, with a secondary evolved away from the main sequence star. 2. AP Aur is a deep-contact binary with the extreme mass ratio, so it is instable. It probably coaleses to be a single star, or evolves into a cataclys- mic variable by lossing the common envelope. |
| 语种 | 中文 |
| 学科主题 | 天文学 |
| 公开日期 | 2016-05-03 |
| 页码 | 86 |
| 内容类型 | 学位论文 |
| 源URL | [http://ir.ynao.ac.cn/handle/114a53/4359]  |
| 专题 | 云南天文台_其他 |
| 推荐引用方式 GB/T 7714 | 李立芳. 密近双星的演化链[D]. 昆明. 中国科学院云南天文台. 1998. |
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