YNAO OpenIR  > 双星与变星研究组
大质量双星轨道周期的分析研究
赵二刚
Subtype硕士
Thesis Advisor钱声帮
2010-06-07
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大质量双星 测光观测 周期分析 双星物质交流 双星结构和演化
Abstract大质量双星是指子星的光谱型早于B5型的OB型双星,其研究对了解密近双星质量及角动量的交流和损失以及双星的演化有着重要的意义。本文对大质量双星进行了初步的统计分析,并对部分大质量双星进行了观测研究,取得了如下的研究结果: 1、发现O型大质量相接双星LY Aur的轨道周期在长期增加的基础上叠加了一个周期为13.1年的周期性变化,增加率为dP/dt =3.02 ×10−7days/year。周期的长期增加是由次星向主星的物质交流引起的,这说明该系统正处于以次星的核反应时标进行的Case A慢速物质交流阶段。轨道周期的周期性变化可以用第三天体的光时轨道效应来解释,通过计算得到的第三天体质量下限为4.02个太阳质量。 2、对B型大质量相接双星RZ Pyx的O−C分析得到其轨道周期在长期增加的基础上叠加了一个周期为46.2年的周期性变化。轨道周期的长期增加是由次星向主星转移物质和主星的星风物质损失共同作用造成的,这可能使RZ Pyx向相接度更浅的方向演化,甚至可能导致相接破裂。用第三天体的光时轨道效应来解释RZ Pyx轨道周期的周期性变化,可以计算出第三天体可能是一质量为0.3个太阳质量的冷星。 3、对B型大质量半相接双星AI Cru进行观测分析,同样发现轨道周期存在长期增加,表明其处于以次星核反应时标进行的Case A慢速物质交流阶段,周期的长期增加可能是由次星向主星转移物质和主星的星风物质损失共同造成的。对光电和 CCD的观测数据分析表明,轨道周期还存在周期性变化成分,该周期性变化可以用质量为0.2个太阳质量的额外天体的光时轨道效应来解释。
Other AbstractMassive binary in this paper is the kind of binary, whose spectral type is earlierthan B5. Research on massive binary plays an important role in the mass and angular momentum transfer or loss between the components, and the evolution of binary. This paper does some statistics and analysis on the massive binary, some massive binaries are observed and analyzed. The results are obtained as follows: 1.It is discovered that the period of the O type binary LY Aur is increasing continuously at a rate of dP/dt =3.02 × 10−7days/year and a cyclic oscillation with a period of 13.1 years. The long-term period increase can be explained by the mass transfer from the less massive component to the more one, which indicates that the system is undergoing a Case A slow mass-transfer stage on the nuclear time scale of the secondary. The periodic change may be due to the light-travel time effect of the third component and the lowest mass of the third body is computed to be 4.02Msun. 2.Based on the O−C analysis of the B-type massive contact binary RZ Pyx, we find a cyclic period change of 46.2 years superimposed on a long-term increasing. The long-term increasing of orbital period is caused by the mass transfer from the secondary to the primary and the mass loss from the primary by the stellar wind. It possible makes RZ Pyx evolve to the direction of more shallower contact degree and the contact may be broken finally. The cyclic change of orbital period may be caused by the light-travel time effect of the third body, and this component may be a cool star with a mass of 0.3Msun . 3.It is found the orbital period of B-type semi-detached binary AI Cru has a long-term increasing, which indicates that the system is undergoing a Case A slow mass-transfer stage on the nuclear time scale of the secondary. The mass transfer from the secondary to the primary and the mass loss from the primary is the reason why the period is increasing. Analysis on the photoelectric and CCD data displays a cyclic change, and can be explained by the light-travel time effect of the third body with a lowest mass of 0.2Msun .
Subject Area天文学
Pages57
Language中文
Document Type学位论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/5976
Collection双星与变星研究组
Recommended Citation
GB/T 7714
赵二刚. 大质量双星轨道周期的分析研究[D]. 北京. 中国科学院研究生院(云南天文台),2010.
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