【摘要】：AF型相接雙星是指含有一個(gè)光譜型為A型或者F型子星的相接雙星系統(tǒng),它們是連接早型和晚型相接雙星的橋梁,在相接雙星樣本中具有重要地位。AF型相接雙星具有周期短(通常小于1天),亮度大等易于觀測的特點(diǎn)。本文選取了F型相接雙星V502 Oph,MQ UMa,II UMa,NO Cam,V776Cas和A型相接雙星V868 Mon及A型近相接雙星V921 Her為樣本,利用云南天文臺1m和60cm望遠(yuǎn)鏡,興隆觀測站85cm望遠(yuǎn)鏡等設(shè)備對這些源進(jìn)行長期監(jiān)測,獲得其光變曲線和光極小時(shí)刻數(shù)據(jù)。然后,利用2013版的W-D程序及O-C方法對得到的觀測資料進(jìn)行解軌分析和周期變化研究,獲得雙星系統(tǒng)的基本物理參量,兩子星間相互作用情況及其周圍可能存在的第三天體等信息。1.研究表明,MQ UMa、II UMa和V776 Cas均為小質(zhì)量比深度相接雙星系統(tǒng),它們可能是藍(lán)離散星等特殊天體的前身星。結(jié)合小質(zhì)量比深度相接雙星的統(tǒng)計(jì)資料,我們發(fā)現(xiàn)AF型星中小質(zhì)量比深度相接雙星的形成率非常高,它們是研究雙星并合和特殊天體形成等問題的重要樣本;2.本文選取的上述七個(gè)樣本中,僅晚F型相接雙星V502 Oph光變曲線表現(xiàn)出畸變,需要用黑子模型來擬合,其余目標(biāo)源的光變曲線對稱性均很好,說明與晚型相接雙星相比,AF型相接雙星系統(tǒng)中磁活動較弱,恒星表面對流層較薄;3.本文對所有獲得絕對物理參量的AF型相接雙星進(jìn)行統(tǒng)計(jì),根據(jù)系統(tǒng)中兩子星現(xiàn)有的質(zhì)量和光度估算出了它們的初始質(zhì)量。對AF型相接雙星系統(tǒng)中兩子星初始質(zhì)量的統(tǒng)計(jì)分析表明,決定其最終演化成A次型還是W次型系統(tǒng)的主要因素是雙星系統(tǒng)中兩子星的初始質(zhì)量和,初始質(zhì)量較大的系統(tǒng)(約3.1M)演化成為A次型系統(tǒng),而初始質(zhì)量較小的系統(tǒng)(約2.5M)演化成為W次型系統(tǒng)。AF型系統(tǒng)中初始質(zhì)量較大的子星先演化充滿其洛希瓣,然后向初始質(zhì)量較小的子星轉(zhuǎn)移物質(zhì),經(jīng)過質(zhì)量比反轉(zhuǎn),初始質(zhì)量較大的子星最終成為小質(zhì)量子星。初始質(zhì)量較大的子星損失物質(zhì)的30%到50%轉(zhuǎn)移給了現(xiàn)在的大質(zhì)量星,其余均以星風(fēng)物質(zhì)損失的形式逃離雙星系統(tǒng);4.結(jié)合測光、分光、O-C分析的結(jié)果,作者發(fā)現(xiàn)V502 Oph,MQ UMa,NO Cam,V776 Cas以及V921 Her周圍都有第三天體存在。對AF型相接雙星伴星天體的統(tǒng)計(jì)研究表明,光時(shí)軌道效應(yīng)和測光解軌是證實(shí)第三天體存在的主要手段,而通過光時(shí)軌道效應(yīng)證實(shí)第三天體存在是最可靠和最常用的方法。在已經(jīng)研究的AF型相接雙星中,約有60%的系統(tǒng)已經(jīng)被證實(shí)存在第三天體,而實(shí)際上這一比重可能會更高。這說明第三天體在AF型相接雙星系統(tǒng)中是普遍存在的。在本文選取的所有目標(biāo)源中,NO Cam的第三天體離其宿主雙星的距離最近(2AU)。這些資料的積累,為研究第三天體在雙星形成和演化中扮演的作用提供了重要的實(shí)測依據(jù);5.雙星系統(tǒng)的軌道周期變化(增加或減小),是雙星系統(tǒng)動力學(xué)相互作用的直接體現(xiàn)。在本文研究的樣本中,V502 Oph周期在減小,II UMa,NO Cam,V868 Mon及V921 Her周期均在增加。本文共收集了23顆軌道周期持續(xù)增加(減小)的AF型相接雙星系統(tǒng),為將來進(jìn)一步的分析研究積累了豐富的資料。
[Abstract]:The AF-type phase-connected binary is a two-star system with a spectral type of type A or F, which is a bridge connecting the early and late-type connecting binary, and has an important position in the sample of the two-star. The AF-type phase-connected binary has the characteristics of short period (usually less than 1 day), high brightness and the like. In this paper, the F-type phase-connected binary V502 Oph, the MQ UMa, the II UMa, the NO Cam, the V776Cas and the A-type phase-connected binary V868Mon and the A-type near-phase double-star V921 Her are selected as the samples, and these sources are monitored for a long time by the equipment such as the 1 m and the 60 cm telescope of the Yunnan Observatory and the 85cm telescope of the Xinglong Observatory. And obtaining the light change curve and the light minimum time data. Then, using the W-D program of 2013 and the O-C method to study the orbit analysis and the periodic variation of the obtained observation data, the basic physical parameters of the binary system, the interaction between the two sub-stars and the third celestial bodies which may exist around them are obtained. The results show that the MQ UMa, II UMa and V776 Cas are both small mass-to-depth and deep-connected binary systems, which may be the precursor of a special celestial body such as a blue discrete star. In this paper, we find that the formation rate of the small and medium mass of the AF-type star is very high, which is an important sample for studying the formation of the double-star and the formation of special celestial bodies. In the above seven samples, only the late F-type phase-connected binary V502 Oph photorefractive curve shows the distortion, and it is necessary to use the sunspot model to fit. The symmetry of the photorefractive curves of the other target sources is good, which indicates that the magnetic activity in the AF-type phase-connected binary system is weak compared with the late-type phase-connected binary star. The surface of the star is relatively thin;3. In this paper, all AF-type phase-connected binary systems with absolute physical parameters are counted, and their initial quality is estimated according to the existing quality and luminosity of the two sub-stars in the system. The statistical analysis of the initial mass of the two sub-stars in the AF-type phase-connected double-star system shows that the main factors of determining the initial mass of the two-star system and the W-type system in the two-star system are the initial quality of the two sub-stars in the double-star system and the evolution of the system (about 3.1 M) with a large initial mass into the A-type system. The system with less initial mass (about 2.5M) has evolved into a W-type system. In the AF-type system, the initial mass of the sub-star is full of its loxi-lobe, and then the sub-star with smaller initial mass is transferred to the sub-star with smaller initial mass, and the sub-star with larger initial mass is finally the small-quality sub-star after the mass ratio is reversed. The 30% to 50% of the mass of the initial mass of the sub-star is transferred to the present mass star, the rest of which escapes the binary system in the form of loss of the star-like material; Combined with the results of photometry, spectrophotometry, and O-C analysis, the authors found that the presence of a third object in V502 Oph, MQ UMa, NO Cam, V776 Cas, and V921 Her. The statistical study of the AF-type phase-connected binary-satellite object shows that the light-track effect and the light-metering solution are the main means to confirm the existence of the third object, and the existence of the third object is the most reliable and most common method through the light-track effect. In the AF-type phase-connected binary that has been studied, about 60% of the system has been confirmed to have a third object, and in effect this specific gravity may be higher. This indicates that the third object is ubiquitous in the AF-type phase-connected binary system. In all the target sources selected herein, the third object of NO Cam is closest to its host binary (2AU). The accumulation of these data provides an important basis for the study of the role of the third object in the formation and evolution of the double star. The orbital period change (increase or decrease) of the double-star system is a direct reflection of the dynamic interaction of the binary system. In the samples studied here, the V502 Oph cycle is decreasing, and the II, UMa, NO Cam, V868 Mon, and V921 Her cycles are increasing. In this paper, the AF-type phase-connected binary system with a continuous increase (decrease) of 23 orbital periods is collected, and a lot of data has been accumulated for further analysis and research in the future.
【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】：博士
【學(xué)位授予年份】：2016
【分類號】：P153

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