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大麦哲伦星云中早型相接双星的分析与研究
其他题名Analysis and study of early-type contact binaries in the Large Magellanic Cloud
马文武
学位类型硕士
导师钱声帮
2022-07-01
学位授予单位中国科学院大学
学位授予地点北京
培养单位中国科学院云南天文台
学位专业天体物理
关键词大麦哲伦星云 早型星 相接双星 物理参数
摘要大麦哲伦星云中早型相接双星是指由光谱型为O、B和A型的两子星均充满各自的洛希瓣且具有对流公共包层的相互作用双星系统。由于两子星非常靠近,星风物质损失、物质的转移和交流以及吸积过程使得相接双星的演化明显区别于单星。同时,大麦哲伦星云的贫金属性又为早型相接双星的形成和演化增加了神秘色彩。在最近的二十年中,许多基于光学引力透镜的巡天项目,例如OGLE、MACHO、EROS已经在大麦哲伦星云中发现了成千上万个不同类型的掩食双星。不同的项目都留下了庞大的观测数据库,这对研究各种类型的食双星都有重要意义。在大麦哲伦星云中部分早型分离双星被用于测量星系的几何距离,具有较高偏心率的食双星用来研究拱线运动,部分大质量相接或近相接双星被用于研究周期-光度-颜色关系,对周期在20-50天 的一些B型食双星研究,得到了相关物理参数、质量比分布的统计关系以及它们演化。然而,早型相接双星的研究几乎是一个空白。依托OGLE项目的1.3米光学引力透镜巡天望远镜,我们对大麦哲伦星云中497个相接双星的研究,得到它们的物理参数(例如质量、半径、光度、温度、轨道倾角、相接度等等),分析它们的演化轨迹,确定系统的年龄,统计它们的周期-颜色-光度关系以及质量比的分布将是对研究空白极大的填充,也是目前这一研究领域迫在眉睫的问题。而且,大麦哲伦星云中早型相接双星足够的明亮,它们的轨道周期相对较短,这使得它们即使在短时间的观测中也很容易被发现。综上所述,大麦哲伦星云是研究早型相接双星最理想的天体物理实验室。本文在OGLE四期数据中选择了497个相接双星作为研究样本,对研究样本分析后发现,I波段星等范围为12.73 mag至19.898 mag ,V 波段星等范围在13.187 mag 至20.598 mag 之间,V-I色指数范围为-0.217 mag 至 2.774 mag, V-I 的峰值在0.1附近的占了样本的一半,说明大部分为早型星。通过对颜色星等图的分析,发现大部分样本位于主序带上。样本的轨道周期范围从0.13564天到126 d,周期峰值在0.8天 附近。基于以下条件从497个样本中选择了32个早型相接双星作为研究目标,(1):V-I的值在-0.2附近至0之间;(2)轨道周期在0.8 天左右;(3)两极小几乎等深且光变曲线具有典型的EW类型。为了了解这32个研究目标的几何结构和演化状态,对其中四个目标源利用W-D程序对其V、I波段的光变曲线进行了分析,给出了它们的测光参数,例如轨道倾角、质量比、周期以及相接度等。大麦哲伦星云中恒星的金属丰度明显低于太阳的金属丰度,金属丰度的不同使得恒星的形成与演化存在联系与差异,因此第二项工作选择了银河系内的TW Cas这个源,对它进行了测光研究。TW Cas是一个由B型星和类太阳恒星组成的食双星系统,具有轨道周期P=1.42832665 d以及质量比q=0.4873。基于TESS观测到的最新光变曲线,利用W-D程序获得了TW Cas的轨道参数,我们发现次星充满其洛希瓣,而主星的相接度只有16.08%,次星的温度和质量低于主星,但是演化的反而快,因此TW Cas是典型的Algol双星。$O-C$曲线呈现向上的抛物线变化,同时叠加了振幅为0.024585d,周期为113.41年的周期振荡。向上的抛物线变化表明轨道周期长期增加,说明该系统中存在从次星到主星的快速物质转移过程。周期振荡可能是由于存在第三天体的光时轨道效应引起的。
其他摘要Early-type contact binaries in the Large Magellanic Cloud are interacting binary systems consisting of two stars of spectral types O, B and A that both fill their respective Roche lobes and share a common envelope. Secondly, the metal abundance of the Large Magellanic Cloud is significantly lower than that of the solar, which adds to the mystery of the formation and evolution of early-type contact binaries. In the last two decades, Optical Gravitational Lensing Experiment project such as OGLE, MACHO, and EROS have discovered thousands of different types of eclipsing binaries in the Large Magellanic Cloud. The different projects have left a huge database of observations, which is important for the study of all types of eclipsing binaries. Some of the early-type detached binaries in the Large Magellanic Cloud have been used to measure the geometric distances of galaxies. Eclipsing binaries with high eccentricity are used to study the Apsidal Motions. Partially massive contact or near-contact binaries have been used to study the period-luminosity-color relation. A number of B-type eclipsing binaries with periods of 20-50 days have been studied to obtain the relevant physical parameters, statistical relations of the mass ratio distribution, and their evolution. However, the study of early-type contact binaries is almost a gap. Relying on the 1.3-m optical gravitational lensing survey telescope of the OGLE project, our study of 497 contact binaries in the Large Magellanic Cloud, obtaining their physical parameters (e.g. mass, radius, luminosity, temperature, orbital inclination, conjunctions, etc.), analyzing their evolutionary trajectories, determining the age of the system, and accounting for their period-color-luminosity relations and mass ratio distribution will be a great help to study the gap will be greatly filled and is an urgent problem in this research field. The early-type contact binaries in the Large Magellanic Cloud are bright enough, while their relatively short orbital periods make them easy to detect even in short observations. In summary, the Large Magellanic Cloud becomes the ideal astrophysical laboratory to study early-type contact binaries.We selected 497 contact binaries in the OGLE-IV data as the study sample. The I-band magnitude range of objects presented in our sample is from 12.73 mag to 19.898 mag. The V-band magnitude range of objects presented in our sample is from 13.187 mag to 20.598 mag. The V-I ranges from -0.217 mag to 2.774 mag, with the peak of V-I around 0.1, which accounts for half of the sample, indicating that most are early-type stars. By analyzing the color–magnitude diagram, we find that most of the sample is located on the main sequence. The orbital period of the sample ranges from 0.13564 to 126 days, with a peak around 0.8 days. Thirty-two early-type contact binaries were selected as study targets from a sample of 497 based on the following requirements: (1) V-I values between -0.2 and 0; (2) orbital periods of about 0.8 days; and (3) two poles of almost equal depth and typical EW type light curves. To understand its geometrical structure and evolutionary state, the V and I light curves were analyzed using the W–D method.The metal abundances of stars in the Large Magellanic Cloud are significantly lower than those of the Sun, and there are links and differences in whether the differences in metal abundances have a bearing on star formation and evolution. Therefore, the second work chose TW Cas in the Milky Way for its photometric study. TW Cas is an eclipsing binary that contains B-type and solar-like components with an orbital period of 1.42832665 d and mass ratio of 0.4873. The semi-detached configuration makes it a key goal for understanding Algol-type eclipsing binaries evolution. However, the physical parameters and evolutionary state of TW Cas are still unknown. W–D differential correction program was employed to give orbital parameters and configuration and extend our knowledge of TW Cas evolution. We present light curves and 64 eclipsing times observed by Transiting Exoplanet Survey Satellite (TESS) telescope. Photometric analyses of the TESS light curve suggest that TW Cas is a semi-detached system where the less massive component is filling its critical Roche lobe, and a large dark spot is found on the polar of the less massive one. By using all light minima times, it is detected that the O-C curve shows an upward parabolic change while a cyclic oscillation is superimposed with an amplitude of 0.024585 days and a period of 113.41 yr. The upward parabolic change may indicate a long-term increase of the orbital period at a rate of , which reveals a rapid mass transfer between the components. The cyclic oscillation might result from the light-travel-time effect owing to the presence of a third body. The semi-detached configuration that less mass component fills its Roche lobe, together with the long-term increase of orbital period and the presence of a large dark spot on the less massive component indicates that TW Ca is at a critical stage of evolution after a mass ratio inversion.
学科领域天文学 ; 恒星与银河系
学科门类理学 ; 理学::天文学
页数0
语种中文
文献类型学位论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/25773
专题双星与变星研究组
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马文武. 大麦哲伦星云中早型相接双星的分析与研究[D]. 北京. 中国科学院大学,2022.
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