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  本文選題：密近雙星　切入點：黑子活動　出處：《湘潭大學(xué)》2016年碩士論文

【摘要】：宇宙中有50%以上的恒星是雙星,其中密近雙星是非常重要的一員。它們常常表現(xiàn)出活躍而復(fù)雜的物理活動,例如色球活動、CaII HK譜線發(fā)射、黑子活動、軌道周期變化等。通過對密近雙星進(jìn)行觀測,并對得到的光變曲線、O-C曲線等進(jìn)行分析計算,我們能夠得到大量有用的信息,為我們研究天體的結(jié)構(gòu)、演化、相互作用等提供了有利條件。本文首先對雙星的綜合光變曲線分析法和軌道周期變化的基本研究方法進(jìn)行了簡單介紹,然后分別對三顆樣本星RT CrB、GSC 1537-1557與AH Tauri的光變曲線以及軌道周期進(jìn)行了研究。我們得到的主要結(jié)果如下:1.對分離雙星RT CrB 1985年與2001年的光變曲線進(jìn)行了分析,得到了其測光解和黑子活動參量。用主子星上的高溫黑子以及次子星上的低溫黑子對光變曲線進(jìn)行了擬合,較好地解釋了光變曲線的畸變擾動波。同時對RT CrB軌道周期的分析發(fā)現(xiàn)其軌道周期存在長期減小,減小率為7 1dP/dt3.11 10 d yr--=-′,這可能是由星風(fēng)磁滯引起的角動量損失造成的。2.分析了GSC 1537-1557的CCD測光數(shù)據(jù),發(fā)現(xiàn)GSC 1537-1557是一顆W次型的相接雙星,相接度為f=(8.10±1.79)%,兩子星質(zhì)量比為q=M_2/M_1=2.645。其光變曲線的不對稱變化可以由主子星上的高溫黑子與次子星上的低溫黑子來解釋。通過分析O-C曲線我們發(fā)現(xiàn)GSC 1537-1557的軌道周期存在周期性變化,周期為8.1年,振幅為0.00335天。這可能是由第三天體的光時軌道效應(yīng)造成的,若取該系統(tǒng)的總質(zhì)量為1.3M_1,則第三天體的質(zhì)量下限為0.19 M,是一個低溫且昏暗的天體。3.從2006年AH Tauri的CCD測光觀測數(shù)據(jù)中,得到了兩個新的光極小時刻,利用W-D程序分析觀測數(shù)據(jù),獲得了軌道測光解,發(fā)現(xiàn)AH Tauri是一顆A次型的W UMa型相接雙星,相接度為6.6%,兩子星質(zhì)量比為0.505,其光變曲線的畸變能夠用主子星上的低溫黑子來解釋。另外,結(jié)合新極小時刻和從文獻(xiàn)中搜集到的極小時刻,我們分析得到AH Tauri的軌道周期具有兩個變化成分,一個是長期減小成分,減小率為dP/dt(1.823(?)0.215)10~(-7)d yr-(-1);另一個為周期性變化成分,變化周期為54.62年。軌道周期的長期變化可能由兩子星間物質(zhì)交流或是星風(fēng)磁滯引起的系統(tǒng)質(zhì)量損失造成,相應(yīng)的物質(zhì)交流率為dM_1/dt1.94×10~(-7)M yr~(-1),星風(fēng)磁滯引起系統(tǒng)的質(zhì)量損失率為dM/dt--4.97×10~(-11)Myr~(-1)。周期性震蕩可由第三天體的光時軌道效應(yīng)或是活動子星的周期性磁活動來解釋。
[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 鹵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.
【學(xué)位授予單位】：湘潭大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2016
【分類號】：P153
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本文編號：1697047