AF型相接双星的观测与研究
发布时间：2019-05-17 01:15
【摘要】：AF型相接双星是指含有一个光谱型为A型或者F型子星的相接双星系统,它们是连接早型和晚型相接双星的桥梁,在相接双星样本中具有重要地位。AF型相接双星具有周期短(通常小于1天),亮度大等易于观测的特点。本文选取了F型相接双星V502 Oph,MQ UMa,II UMa,NO Cam,V776Cas和A型相接双星V868 Mon及A型近相接双星V921 Her为样本,利用云南天文台1m和60cm望远镜,兴隆观测站85cm望远镜等设备对这些源进行长期监测,获得其光变曲线和光极小时刻数据。然后,利用2013版的W-D程序及O-C方法对得到的观测资料进行解轨分析和周期变化研究,获得双星系统的基本物理参量,两子星间相互作用情况及其周围可能存在的第三天体等信息。1.研究表明,MQ UMa、II UMa和V776 Cas均为小质量比深度相接双星系统,它们可能是蓝离散星等特殊天体的前身星。结合小质量比深度相接双星的统计资料,我们发现AF型星中小质量比深度相接双星的形成率非常高,它们是研究双星并合和特殊天体形成等问题的重要样本;2.本文选取的上述七个样本中,仅晚F型相接双星V502 Oph光变曲线表现出畸变,需要用黑子模型来拟合,其余目标源的光变曲线对称性均很好,说明与晚型相接双星相比,AF型相接双星系统中磁活动较弱,恒星表面对流层较薄;3.本文对所有获得绝对物理参量的AF型相接双星进行统计,根据系统中两子星现有的质量和光度估算出了它们的初始质量。对AF型相接双星系统中两子星初始质量的统计分析表明,决定其最终演化成A次型还是W次型系统的主要因素是双星系统中两子星的初始质量和,初始质量较大的系统(约3.1M)演化成为A次型系统,而初始质量较小的系统(约2.5M)演化成为W次型系统。AF型系统中初始质量较大的子星先演化充满其洛希瓣,然后向初始质量较小的子星转移物质,经过质量比反转,初始质量较大的子星最终成为小质量子星。初始质量较大的子星损失物质的30%到50%转移给了现在的大质量星,其余均以星风物质损失的形式逃离双星系统;4.结合测光、分光、O-C分析的结果,作者发现V502 Oph,MQ UMa,NO Cam,V776 Cas以及V921 Her周围都有第三天体存在。对AF型相接双星伴星天体的统计研究表明,光时轨道效应和测光解轨是证实第三天体存在的主要手段,而通过光时轨道效应证实第三天体存在是最可靠和最常用的方法。在已经研究的AF型相接双星中,约有60%的系统已经被证实存在第三天体,而实际上这一比重可能会更高。这说明第三天体在AF型相接双星系统中是普遍存在的。在本文选取的所有目标源中,NO Cam的第三天体离其宿主双星的距离最近(2AU)。这些资料的积累,为研究第三天体在双星形成和演化中扮演的作用提供了重要的实测依据;5.双星系统的轨道周期变化(增加或减小),是双星系统动力学相互作用的直接体现。在本文研究的样本中,V502 Oph周期在减小,II UMa,NO Cam,V868 Mon及V921 Her周期均在增加。本文共收集了23颗轨道周期持续增加(减小)的AF型相接双星系统,为将来进一步的分析研究积累了丰富的资料。
[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.
【学位授予单位】：中国科学院研究生院(云南天文台)
【学位级别】：博士
【学位授予年份】：2016
【分类号】：P153
本文编号：2478692
[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.
【学位授予单位】：中国科学院研究生院(云南天文台)
【学位级别】：博士
【学位授予年份】：2016
【分类号】：P153
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