Am食雙星的觀測(cè)與研究
發(fā)布時(shí)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)。化學(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(duì)Am食雙星的觀測(cè)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(duì)CP星進(jìn)行了簡(jiǎn)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(gè)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(gè)周期小于一天的Am食雙星V1073Cyg和TYC6408-989-1進(jìn)行觀測(cè)研究,主要結(jié)果如下:1、我們對(duì)Am食雙星進(jìn)行調(diào)研補(bǔ)充,發(fā)現(xiàn)17個(gè)Am食雙星未在73個(gè)Am食雙星之列,并將其列在Am食雙星增補(bǔ)表中,給出其周期和光譜型等信息。我們對(duì)Am食雙星的周期進(jìn)行統(tǒng)計(jì)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(zhǎng)周期則比較少,周期小于一天的也比較少,目前只有四個(gè)系統(tǒng),即:TYC6408-989-1、V1073Cyg、V2787Ori和IW Per。其中IW Per為增補(bǔ)的Am食雙星之一。2、對(duì)W UMa型Am食雙星V1073Cyg進(jìn)行測(cè)光觀測(cè)、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(shí)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(dòng)量損失的綜合效應(yīng)所致。同時(shí),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(shí)軌道效應(yīng)引起的。光變曲線分析顯示該系統(tǒng)是一個(gè)過相接雙星系統(tǒng),探測(cè)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(gè)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(duì)該系統(tǒng)進(jìn)行了首次的測(cè)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(gè)臨近相接的密近雙星系統(tǒng)。我們將進(jìn)一步對(duì)該系統(tǒng)進(jìn)行觀測(cè),以期獲得多波段的觀測(cè)數(shù)據(jù)對(duì)其進(jìn)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(guó)科學(xué)院研究生院(云南天文臺(tái))
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2016
【分類號(hào)】：P144.9
本文編號(hào)：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(guó)科學(xué)院研究生院(云南天文臺(tái))
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2016
【分類號(hào)】：P144.9
【相似文獻(xiàn)】
相關(guān)期刊論文 前10條
1 茶光偉;譚徽松;李曉渝;彭松泉;;五個(gè)食雙星系統(tǒng)的Hα食外光譜[J];天文學(xué)報(bào);1988年03期
2 李林森;;引力常數(shù)隨時(shí)間變化對(duì)雙星(密近食雙星)軌道演變的影響(圓形軌道情形)[J];天文研究與技術(shù);2010年04期
3 陸文賢;食雙星的分光軌道解:WX Cnc[J];Chinese Journal of Astronomy and Astrophysics;1990年03期
4 陸文賢;食雙星的分光軌道解:AA UMa[J];Chinese Journal of Astronomy and Astrophysics;1988年01期
5 陸文賢;食雙星的分光軌道解:BD+37°2356[J];Chinese Journal of Astronomy and Astrophysics;1988年04期
6 皮青峰;張立云;程長(zhǎng)青;;相接食雙星GR Boo極小時(shí)刻的分析研究[J];貴州大學(xué)學(xué)報(bào)(自然科學(xué)版);2013年06期
7 李燕俠;向茂盛;朱輝;付建寧;張燕平;;食雙星仙女座BX軌道周期長(zhǎng)時(shí)標(biāo)變化的觀測(cè)研究[J];北京師范大學(xué)學(xué)報(bào)(自然科學(xué)版);2011年02期
8 翟迪生;黃寅亮;;天龍座食雙星RZ周期的長(zhǎng)期變化及其測(cè)光軌道解[J];天文學(xué)報(bào);1980年02期
9 劉學(xué)富,彭松泉,茶光偉;食雙星32Cyg 1981年食的光譜觀測(cè)和分析[J];Chinese Journal of Astronomy and Astrophysics;1984年03期
10 劉學(xué)富,彭松泉,茶光偉;食雙星31 Cyg 1982年食期間的視向速度和大氣食效應(yīng)[J];科學(xué)通報(bào);1984年09期
相關(guān)博士學(xué)位論文 前1條
1 張立云;晚型食雙星磁活動(dòng)的觀測(cè)研究[D];中國(guó)科學(xué)院研究生院（云南天文臺(tái)）;2008年
相關(guān)碩士學(xué)位論文 前2條
1 潘洋;疏散星團(tuán)NGC 869中的EB型食雙星測(cè)光研究[D];西華師范大學(xué);2016年
2 田曉慢;Am食雙星的觀測(cè)與研究[D];中國(guó)科學(xué)院研究生院(云南天文臺(tái));2016年
，本文編號(hào)：2389016
本文鏈接：http://sikaile.net/kejilunwen/tianwen/2389016.html
最近更新
教材專著
