密近双星RT CrB、GSC 1537-1557与AH Tauri的测光研究与轨道周期分析

发布时间：2018-04-01 19:48

  本文选题：密近双星　切入点：黑子活动　出处：《湘潭大学》2016年硕士论文

【摘要】：宇宙中有50%以上的恒星是双星,其中密近双星是非常重要的一员。它们常常表现出活跃而复杂的物理活动,例如色球活动、CaII HK谱线发射、黑子活动、轨道周期变化等。通过对密近双星进行观测,并对得到的光变曲线、O-C曲线等进行分析计算,我们能够得到大量有用的信息,为我们研究天体的结构、演化、相互作用等提供了有利条件。本文首先对双星的综合光变曲线分析法和轨道周期变化的基本研究方法进行了简单介绍,然后分别对三颗样本星RT CrB、GSC 1537-1557与AH Tauri的光变曲线以及轨道周期进行了研究。我们得到的主要结果如下:1.对分离双星RT CrB 1985年与2001年的光变曲线进行了分析,得到了其测光解和黑子活动参量。用主子星上的高温黑子以及次子星上的低温黑子对光变曲线进行了拟合,较好地解释了光变曲线的畸变扰动波。同时对RT CrB轨道周期的分析发现其轨道周期存在长期减小,减小率为7 1dP/dt3.11 10 d yr--=-′,这可能是由星风磁滞引起的角动量损失造成的。2.分析了GSC 1537-1557的CCD测光数据,发现GSC 1537-1557是一颗W次型的相接双星,相接度为f=(8.10±1.79)%,两子星质量比为q=M_2/M_1=2.645。其光变曲线的不对称变化可以由主子星上的高温黑子与次子星上的低温黑子来解释。通过分析O-C曲线我们发现GSC 1537-1557的轨道周期存在周期性变化,周期为8.1年,振幅为0.00335天。这可能是由第三天体的光时轨道效应造成的,若取该系统的总质量为1.3M_1,则第三天体的质量下限为0.19 M,是一个低温且昏暗的天体。3.从2006年AH Tauri的CCD测光观测数据中,得到了两个新的光极小时刻,利用W-D程序分析观测数据,获得了轨道测光解,发现AH Tauri是一颗A次型的W UMa型相接双星,相接度为6.6%,两子星质量比为0.505,其光变曲线的畸变能够用主子星上的低温黑子来解释。另外,结合新极小时刻和从文献中搜集到的极小时刻,我们分析得到AH Tauri的轨道周期具有两个变化成分,一个是长期减小成分,减小率为dP/dt(1.823(?)0.215)10~(-7)d yr-(-1);另一个为周期性变化成分,变化周期为54.62年。轨道周期的长期变化可能由两子星间物质交流或是星风磁滞引起的系统质量损失造成,相应的物质交流率为dM_1/dt1.94×10~(-7)M yr~(-1),星风磁滞引起系统的质量损失率为dM/dt--4.97×10~(-11)Myr~(-1)。周期性震荡可由第三天体的光时轨道效应或是活动子星的周期性磁活动来解释。
[Abstract]:More than 50% of the stars in the universe are binary stars, of which close binaries are very important.They often exhibit active and complex physical activities, such as chromospheric activities such as the emission of CaII HK spectral lines, sunspot activities, orbital cycle variations, and so on.Through the observation of close binaries and the analysis and calculation of the optical variation curves and O-C curves, we can get a lot of useful information, which provides favorable conditions for us to study the structure, evolution and interaction of celestial bodies.In this paper, the comprehensive phototropic curve analysis of binary stars and the basic research methods of orbital periodic variation are briefly introduced, and then the phototropic curves and orbital periods of three sample stars, RT CrBGSC1537-1557 and AH Tauri, are studied respectively.Our main results are as follows: 1.The photoluminescence curves of RT CrB in 1985 and 2001 are analyzed, and the photometric solutions and sunspot activity parameters are obtained.The high temperature sunspot on the main substar and the low temperature sunspot on the secondary substar are used to fit the light variation curve, and the distortion disturbance wave of the light variation curve is well explained.At the same time, it is found that the orbital period of RT CrB decreases for a long time, and the decreasing rate is 7 1dP/dt3.11 10 d / y ~ (-1), which may be caused by the angular momentum loss caused by the wind hysteresis.The CCD photometry data of GSC 1537-1557 are analyzed. It is found that the GSC 1537-1557 is a W type intersected binary star with a degree of connection of 8.10 卤1.79 and a mass ratio of QM _ 2 / M _ 1 / M _ 1 / 2.645.The asymmetrical variation of the light variation curve can be explained by the high temperature sunspots on the main substar and the low temperature sunspot on the secondary substar.By analyzing the O-C curve, we find that the orbit period of GSC 1537-1557 varies periodically with a period of 8.1 years and an amplitude of 0.00335 days.If the total mass of the system is 1.3 M-1, the lower mass limit of the third celestial body is 0.19 m, which is a low temperature and dim object.From the CCD photometry data of AH Tauri in 2006, two new light minimums are obtained. Using W-D program to analyze the observed data, the orbital photometry solution is obtained. It is found that the AH Tauri is a W UMa double star of order A.The degree of connection is 6.6 and the mass ratio of the two sub-stars is 0.505.The distortion of the light variation curve can be explained by the low-temperature sunspots on the main star.In addition, combining the new minimal moment and the minimal time collected from the literature, we obtained that the orbital period of the AH Tauri has two changing components, one is the long-term decreasing component, the reduction rate is dP/dt(1.823(?)0.215)10~(-7)d yr-m-1, and the other is the periodic variation component.The variation period is 54.62 years.The long-term variation of the orbital period may be caused by the mass loss of the system caused by the material exchange between the two subsatellites or by the satellite wind hysteresis. The corresponding mass exchange rate is dM_1/dt1.94 脳 10 ~ (-10) -7 ~ (-7) M ~ (yr) ~ (-1), and the mass loss rate of the system caused by the planetary wind hysteresis is dM/dt--4.97 脳 10 ~ (-10) ~ (-11) ~ (-1).The periodic oscillation can be explained by the optotemporal orbital effect of the third celestial body or the periodic magnetic activity of the active substar.
【学位授予单位】：湘潭大学
【学位级别】：硕士
【学位授予年份】：2016
【分类号】：P153
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本文编号：1697047