YNAO OpenIR  > 双星与变星研究组
食激变变星的测光分析
Alternative TitlePhotometric Study of Eclipsing Cataclysmic Variable Stars
戴智斌
Subtype博士
Thesis Advisor钱声帮
2009-06-01
Degree Grantor中国科学院研究生院(云南天文台)
Place of Conferral北京
Degree Discipline天体物理
Keyword激变变星 双星物质交流 磁滞 演化 类太阳磁活动 光时效应 棕矮星
Abstract激变变星(CVs)是一类相互作用的半相接型密近双星系统,由一颗充满洛希瓣的(K/G/M型)主序矮星或巨星和一颗演化后的白矮星组成。在物质从充满洛希瓣的矮星流向白矮星的过程中,物质流因带有强大的角动量围绕着白矮星运动而无法马上落入白矮星表面,并且彼此之间因粘滞摩擦逐渐消耗角动量而延展形成盘状。这样进入主星洛希瓣的物质流与盘相互碰撞形成了高温高光度的碰撞区域――亮斑。于是,白矮星、吸积盘、亮斑和红矮星就构成了激变变星的基本物理图像。除了偏振星(激变变星的一个磁亚型)以外,几乎所有激变变星的各种观测特征都来自于这个系统内部各成分之间的物理过程和相互作用。在近二十年的激变变星研究领域,轨道周期变化方面的研究工作被长期忽视,主要是由于早期的测光精度不够高,同时激变变星本身比较暗弱且存在大量不规则光变,因此人们在观测上不易获得有价值的数据和重要的研究结果。另一方面,在分光方面的研究也不尽如人意,这是因为激变变星是个含有多光源成分且彼此层次模糊的天体系统,这导致光谱的混叠、偏移和展宽都十分严重而无法获取准确的谱线信息和视向速度曲线。因此,目前要在激变变星领域完成有一定价值的科学研究,无论是测光还是分光都需要有高精度的数据。于是,本篇博士论文立足于国内观测仪器现状,从测光的角度对激变变星中带有掩食的目标进行轨道周期变化分析研究。首先,通过对带有掩食的激变变星进行大量的调研和统计工作,一个较完整的108颗食激变变星星表被获得。其次,以此为基础,对十颗具有代表性特征的食激变变星(新星DQ Her和T Aur,矮新星U Gem、Z Cha和V2051 Oph,类新星AC Cnc、V363 Aur、RW Tri、SW Sex和UU Aqr)进行了重点监测和分析研究。同时,为了更好的开展对激变变星的研究,本篇论文还对带有掩食的激变变星前身星进行详细的调研,并对其中一颗重要的激变变星前身星HW Vir的轨道周期变化和绝对参量进行系统的研究。从这十一颗样本星的分析和早期的统计研究工作中,我们取得了以下三个重要的研究成果: 1. 通过对SW Sex和UU Aqr这两颗处于轨道周期空缺上边缘3h
Other AbstractCataclysmic Variable Stars (CVs) are interactive semi-contact binary systems, which consist of a filled (K/G/M-type) main sequence dwarf or giant and an evolved white dwarf. During the process that materials are transferred from main sequence dwarf to white dwarf, the material stream can not fall on the surface of white dwarf, but go round the white dwarf due to its large angular momentum, and extends to a disk because of viscosity and friction. When the new stream hits the disk, a hot area on the rim of disk can be produced with high luminosity - hot spot. Thus, a physical image for CVs can be constructed by the white dwarf, accretion disk, hot spot and red dwarf. Except for polar (a magnetic subtype of CV), almost all observed characters of CVs are from the physical processes and interaction between all parts of CVs. In recent 20 years, the studies for orbital period changes have been neglected, which is caused by the invalid results from the low precision of photometric data and the observational difficulty for the faint CVs. On the other hand, the spectroscopic data are also disappointed because CVs include many light sources which are hardly distinguished and cause badly pollution, deviation and broadening in spectrum and even stem from the accurate analysis of radial velocity curve. Therefore, in order to make a valid study at present, the photometric or spectroscopic data with high precision are needed. Using the telescopes in China, this paper makes photometric observations for the analysis of orbital period changes of the eclipsing CVs. At first, a complete catalogue of eclipsing CVs including 108 objects is obtained via lots of investigations and statistics. Then, Based on this catalogue, ten representative eclipsing CVs (Novae DQ Her and T Aur, Dwarf Novae U Gem, Z Cha and V2051 Oph, Novae-like AC Cnc, V363 Aur, RW Tri, SW Sex and UU Aqr) are observed and analyzed. At the same time, for the better understand of CVs, this paper still investigates the eclipsing pre-CVs in detail, and makes an analysis of orbital period changes and absolute parameters for an important object - HW Vir. Based on the works of analysis of orbital period changes and statistics for the 11 samples, we obtain three conclusions as follows: 1. According to the studies of orbital period changes on two SW Sex-type stars - SW Sex and UU Aqr, which are located in the range of 3h
Subject Area天文学
Pages202
Language中文
Document Type学位论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/5968
Collection双星与变星研究组
Recommended Citation
GB/T 7714
戴智斌. 食激变变星的测光分析[D]. 北京. 中国科学院研究生院(云南天文台),2009.
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