Am食雙星的觀測與研究
發(fā)布時間：2018-12-21 14:09
【摘要】：Am食雙星是包含有Am型化學(xué)組成特殊星的一類食雙星系統(tǒng)�；瘜W(xué)組成特殊星(Chemically Peculiar Star,即CP星)是一類具有特殊化學(xué)元素豐度的恒星,它們的形成和演化一直是天體物理研究中沒有解決的問題�；瘜W(xué)組成特殊星主要由A型和B型主序星組成,Am型化學(xué)組成特殊星是其中雙星比例最高的一類,可以達(dá)到90%以上,且很多被發(fā)現(xiàn)處于食雙星中。眾所周知,食雙星是人們獲得恒星質(zhì)量、半徑等基本物理參量的重要渠道,通過對Am食雙星的觀測研究,可以得到這類CP星精確的基本物理參量以及物質(zhì)交流等信息,從而更好的研究CP星的起源和演化。本文中我們對CP星進行了簡單綜述,并以2009年Renson和Manfroid發(fā)表的Ap/Am星表為基礎(chǔ),給出了一個目前較為完備的Am食雙星星表。從此星表中,我們選取了兩個周期小于一天的Am食雙星V1073Cyg和TYC6408-989-1進行觀測研究,主要結(jié)果如下:1、我們對Am食雙星進行調(diào)研補充,發(fā)現(xiàn)17個Am食雙星未在73個Am食雙星之列,并將其列在Am食雙星增補表中,給出其周期和光譜型等信息。我們對Am食雙星的周期進行統(tǒng)計分析,發(fā)現(xiàn)其周期分布的峰值是2-4天,其中2-3天分布最多,長周期則比較少,周期小于一天的也比較少,目前只有四個系統(tǒng),即:TYC6408-989-1、V1073Cyg、V2787Ori和IW Per。其中IW Per為增補的Am食雙星之一。2、對W UMa型Am食雙星V1073Cyg進行測光觀測、光變曲線解軌分析以及軌道周期分析。軌道周期分析表明,V1073Cyg的O-C曲線呈現(xiàn)出周期持續(xù)減少的同時疊加周期性震蕩變化。周期減小率約為-4.91(±0.93)×10-8d yr-1。周期減小可能是兩子星間物質(zhì)交流和系統(tǒng)角動量損失的綜合效應(yīng)所致。同時,周期為84.52(±0.52)年、半振幅為4.95(±0.42)AU的周期性震蕩可能是一顆質(zhì)量約為0.488M的第三天體的光時軌道效應(yīng)引起的。光變曲線分析顯示該系統(tǒng)是一個過相接雙星系統(tǒng),探測到其第三光的光度約占系統(tǒng)總光度的20%。光變曲線分析與O-C分析關(guān)于第三天體的結(jié)論很好的符合,這說明此系統(tǒng)很可能是一個Am型三星系統(tǒng)。3、TYC6408-989-1展示出EB型的連續(xù)光變,用麗江70厘米望遠(yuǎn)鏡得到V波段完整光變曲線,我們對該系統(tǒng)進行了首次的測光分析研究。綜合光變曲線解軌分析顯示該系統(tǒng)可以收斂于三種模型,質(zhì)量比范圍為0.205-0.274,它很可能是一個臨近相接的密近雙星系統(tǒng)。我們將進一步對該系統(tǒng)進行觀測,以期獲得多波段的觀測數(shù)據(jù)對其進行詳細(xì)研究。
[Abstract]:Am binary star is a kind of binary star system which contains Am type chemical composition special star. Chemically composed special star (Chemically Peculiar Star, (CP star) is a class of stars with special chemical element abundance. Their formation and evolution has been an unsolved problem in astrophysics. The chemical composition of special stars is mainly composed of A type and B type principal order stars, and Am type chemical composition special stars are the highest proportion of binary stars, can reach more than 90%, and many have been found in the binary stars. As we all know, binary stars are an important way for people to obtain basic physical parameters such as stellar mass and radius. Through the observation and study of Am binary stars, we can obtain the accurate basic physical parameters and material exchange information of this kind of CP stars. Thus, the origin and evolution of CP stars are better studied. In this paper, we give a brief review of CP stars, and based on the Ap/Am catalogue published by Renson and Manfroid in 2009, we present a relatively complete catalogue of binary stars in Am. From this catalog, we selected two Am binary stars, V1073Cyg and TYC6408-989-1, which have a period of less than one day. The main results are as follows: 1. It is found that 17 Am binary stars are not included in the 73 Am binary stars, and they are listed in the supplement table of Am binary stars. The information of their periods and spectral types are given. By statistical analysis of the period of Am binary star, we find that the peak value of the period distribution is 2-4 days, of which 2-3 days are the most, the long period is less, and the period is less than one day. At present, there are only four systems. Namely: TYC6408-989-1,V1073Cyg,V2787Ori and IW Per. Among them, IW Per is one of the supplementary binary stars of Am. The optical measurements of W UMa type Am binary star V1073Cyg, the analysis of optical transformation curve and the analysis of orbital period are carried out. The orbit period analysis shows that the O-C curve of V1073Cyg shows a continuous decrease of period and superimposed periodic oscillation. The period reduction rate is about -4.91 (鹵0.93) 脳 10 ~ (-8) d yr-1.. The decrease of the period may be due to the combined effect of the material exchange between the two subsatellites and the angular momentum loss of the system. At the same time, the periodic oscillation with a period of 84.52 (鹵0.52) years and a half amplitude of 4.95 (鹵0.42) AU may be caused by the photo-time orbital effect of a third celestial body with a mass of about 0.488M. The optical curve analysis shows that the system is an overphase binary system, and the third luminosity of the system is about 20% of the total luminosity of the system. The optical curve analysis is in good agreement with the O-C analysis on the third celestial body, which indicates that the system is probably a Am Samsung system. 3TYC6408-989-1 shows the continuous light variation of the EB model. Using Lijiang 70cm telescope to obtain the complete V band optical curve, we have carried out the first photometric analysis of the system. The results show that the system can converge to three models and the mass ratio ranges from 0.205-0.274. It is very likely that the system is a close binary-star system. We will make further observations of the system in order to obtain multi-band observation data to study it in detail.
【學(xué)位授予單位】：中國科學(xué)院研究生院(云南天文臺)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2016
【分類號】：P144.9
本文編號：2389016
[Abstract]:Am binary star is a kind of binary star system which contains Am type chemical composition special star. Chemically composed special star (Chemically Peculiar Star, (CP star) is a class of stars with special chemical element abundance. Their formation and evolution has been an unsolved problem in astrophysics. The chemical composition of special stars is mainly composed of A type and B type principal order stars, and Am type chemical composition special stars are the highest proportion of binary stars, can reach more than 90%, and many have been found in the binary stars. As we all know, binary stars are an important way for people to obtain basic physical parameters such as stellar mass and radius. Through the observation and study of Am binary stars, we can obtain the accurate basic physical parameters and material exchange information of this kind of CP stars. Thus, the origin and evolution of CP stars are better studied. In this paper, we give a brief review of CP stars, and based on the Ap/Am catalogue published by Renson and Manfroid in 2009, we present a relatively complete catalogue of binary stars in Am. From this catalog, we selected two Am binary stars, V1073Cyg and TYC6408-989-1, which have a period of less than one day. The main results are as follows: 1. It is found that 17 Am binary stars are not included in the 73 Am binary stars, and they are listed in the supplement table of Am binary stars. The information of their periods and spectral types are given. By statistical analysis of the period of Am binary star, we find that the peak value of the period distribution is 2-4 days, of which 2-3 days are the most, the long period is less, and the period is less than one day. At present, there are only four systems. Namely: TYC6408-989-1,V1073Cyg,V2787Ori and IW Per. Among them, IW Per is one of the supplementary binary stars of Am. The optical measurements of W UMa type Am binary star V1073Cyg, the analysis of optical transformation curve and the analysis of orbital period are carried out. The orbit period analysis shows that the O-C curve of V1073Cyg shows a continuous decrease of period and superimposed periodic oscillation. The period reduction rate is about -4.91 (鹵0.93) 脳 10 ~ (-8) d yr-1.. The decrease of the period may be due to the combined effect of the material exchange between the two subsatellites and the angular momentum loss of the system. At the same time, the periodic oscillation with a period of 84.52 (鹵0.52) years and a half amplitude of 4.95 (鹵0.42) AU may be caused by the photo-time orbital effect of a third celestial body with a mass of about 0.488M. The optical curve analysis shows that the system is an overphase binary system, and the third luminosity of the system is about 20% of the total luminosity of the system. The optical curve analysis is in good agreement with the O-C analysis on the third celestial body, which indicates that the system is probably a Am Samsung system. 3TYC6408-989-1 shows the continuous light variation of the EB model. Using Lijiang 70cm telescope to obtain the complete V band optical curve, we have carried out the first photometric analysis of the system. The results show that the system can converge to three models and the mass ratio ranges from 0.205-0.274. It is very likely that the system is a close binary-star system. We will make further observations of the system in order to obtain multi-band observation data to study it in detail.
【學(xué)位授予單位】：中國科學(xué)院研究生院(云南天文臺)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2016
【分類號】：P144.9
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