W UMa型相接双星的观测与研究
发布时间：2018-08-09 19:36
【摘要】：W UMa型双星是一类两子星均充满或超过其洛希瓣并形成公共对流层的相接双星系统。它们所具有的哑铃形结构使得其两子星极易发生相互掩食,展现出连续变化的光变曲线和几乎相等的两食深。同时,共享的对流公共包层使得两子星之间可发生诸如物质与能量的交流和通过外拉格朗日点的物质、能量与角动量的损失等复杂的物理现象。独特的几何结构与这些复杂的物理过程使得W UMa型相接双星成为人们普遍关注的一类天体系统。本论文以W UMa型相接双星为对象,研究了一批样本星的轨道周期变化行为和部分样本星的结构特征与演化状态,得到了如下的一些研究结果:1、对W UMa型相接双星YY Cr B的轨道周期研究表明,该系统既有可能正经历连续的周期衰减,同时伴随着周期的周期性变化,也有可能在过去的20年里经历了一次陡然的周期减小。长期的周期减小可能是由于从主星到次星的质量转移或由恒星风所致的质量损失引起的;而周期性的周期改变应该不是由第三天体的光时轨道效应所致,而应归结于系统的周期性磁活动;另外,陡然的周期减小可能是因陡然的质量转移所致。如果YY CrB的轨道周期确实是长期减小的,那么它将很可能因内外临界洛希瓣收缩而演化成一颗快速旋转单星。2、对两颗低质量比深度相接W UMa型双星V728 Her和AH Aur的轨道周期研究表明:V728 Her的轨道周期连续增长,而AH Aur的轨道周期连续衰减。它们恒定的轨道周期变化暗示着这些双星中的两子星正经历快速的质量转移。依据双星并和理论,并结合蓝离散星和低质量比深度相接双星的观测特征,V728 Her和AH Aur最终可能演化成诸如蓝离散星或FK Com型的快速旋转单星。3、基于V508 Oph的CCD测光观测,我们确定了六个新的光极小时刻,发现了它具有明显不对称的光变曲线。同时,我们的测光解表明它是一颗质量比为q?0.552和相接度为f?15.4%的W UMa型浅度相接双星,不对称的光变曲线应该是次星表面存在活动的热黑子所致。另外,对V508 Oph的轨道周期研究表明它的轨道周期正经历一个多重的复杂变化行为:连续的周期衰减,同时伴随着周期性的周期变化。多重的周期变化行为意味着V508 Oph可能存在周期性的磁活动、两子星间的物质转移和围绕其转动的第三天体。4、通过对V737 Per的首次测光研究,我们发现V737 Per是一颗W次型的浅度相接双星,而观测得到的不对称光变曲线可能是次星表面活动性冷黑子所致。另外,我们首次确定了其测光质量比和相接度。目前,由于可利用的光极小时刻数据仅覆盖了较短的时间范围且没有展现出任何的变化趋势,所以我们当前不能够推断其存在任何可能的周期变化行为,而且其演化状态的确定还需要长期且深入的观测。5、发现浅度相接双星YY Eri的轨道周期存在长期的轨道周期增长的同时附加了一个小幅度的周期性变化。长期的周期增长可能是从小质量次星向大质量主星的物质转移所致,而周期性的周期变化能够归因于第三天体的光时轨道效应或者周期性的磁活动。从长周期的光度变化分析可知,周期性的周期变化很可能是由周期性磁活动所引起。
[Abstract]:The W UMa type binary star is a two star system with two stars filling or exceeding the loxi flap and forming a common troposphere. The dumbbell shaped structures of them make the two stars easily eat each other, show a changing light curve and almost equal two depth of food. There are complex physical phenomena such as the exchange of material and energy and the loss of energy and angular momentum, such as material and energy and the loss of angular momentum. The unique geometric structure and these complex physical processes make W UMa connected binary stars become a class of universal systems of universal concern. This paper is based on W UMa type double stars. The orbital periodic change behavior of a batch of sample stars and the structural features and evolution states of some sample stars are studied. Some results are obtained as follows: 1, the study of the orbit period of W UMa type YY Cr B shows that the system can not only experience continuous periodic decay and decrease, but also can be accompanied by periodic periodic changes of the cycle. It has experienced a steep period reduction over the last 20 years. The long period decrease may be due to mass transfer from the host to the sub star or the mass loss caused by the stellar wind, and the periodic periodic change should not be caused by the optical time orbit effect of the third celestial bodies, and should be attributed to the periodic magnetic activity of the system. In addition, the abrupt period reduction may be caused by abrupt mass transfer. If the orbit cycle of YY CrB is indeed prolonged for a long time, it will probably evolve into a fast rotating single star.2 due to the internal and external critical Loche contraction, and the orbit periodic study of two low mass ratio W UMa double stars V728 Her and AH Aur Ming: the orbit cycle of the V728 Her continues to grow, while the AH Aur's orbital period continuously attenuates. Their constant orbital cycle changes suggest that the two stars in these binary stars are experiencing rapid mass transfer. According to the binary star and theory, the V728 Her and the AH Aur are finally available in conjunction with the observations of the blue discrete star and the low mass ratio of the two stars. We can evolve into a fast rotating single star.3 such as the blue discrete star or FK Com. Based on the CCD measurement of V508 Oph, we have determined six new light moments, and found that it has an obvious asymmetric light curve. At the same time, our photometry shows that it is a shallow connection of a mass ratio of Q? 0.552 and a W UMa type of F? 15.4%. Double stars, asymmetric light curves should be caused by hot spots on the surface of the sub star. In addition, the orbit periodic study of V508 Oph shows that its orbit cycle is experiencing a multiple complex change behavior: continuous periodic decay and periodic periodic variation. Multiple periodic changes mean that V508 Oph can be used. The existence of periodic magnetic activity, the material transfer between the two substars and the third celestial.4 around its rotation, we found that V737 Per is a light connected binary star of a W subtype by the first photometric study of the V737 Per, and the observed asymmetric light curve may be caused by the active cold sunspot on the surface of the substar. In addition, we have made the first confirmation. At present, since the available optical minimum time data is only covered in a short time range and does not show any change trend, we can not infer that there is any possible periodic change at present, and the determination of its evolution state also requires a long and deep observation of.5, It is found that the orbital period of shallow connected binary star YY Eri has a long period of orbital periodic growth and a small amplitude periodic change. The long-term periodic growth may be caused by mass transfer from small mass to mass star, and periodic periodic changes can be attributed to the light time orbit effect of third celestial bodies. Periodic magnetic activity. From the analysis of long-period photometric variation, it can be seen that periodic periodic variation is probably caused by periodic magnetic activity.
【学位授予单位】：湘潭大学
【学位级别】：博士
【学位授予年份】：2016
【分类号】：P153
，
本文编号：2175099
[Abstract]:The W UMa type binary star is a two star system with two stars filling or exceeding the loxi flap and forming a common troposphere. The dumbbell shaped structures of them make the two stars easily eat each other, show a changing light curve and almost equal two depth of food. There are complex physical phenomena such as the exchange of material and energy and the loss of energy and angular momentum, such as material and energy and the loss of angular momentum. The unique geometric structure and these complex physical processes make W UMa connected binary stars become a class of universal systems of universal concern. This paper is based on W UMa type double stars. The orbital periodic change behavior of a batch of sample stars and the structural features and evolution states of some sample stars are studied. Some results are obtained as follows: 1, the study of the orbit period of W UMa type YY Cr B shows that the system can not only experience continuous periodic decay and decrease, but also can be accompanied by periodic periodic changes of the cycle. It has experienced a steep period reduction over the last 20 years. The long period decrease may be due to mass transfer from the host to the sub star or the mass loss caused by the stellar wind, and the periodic periodic change should not be caused by the optical time orbit effect of the third celestial bodies, and should be attributed to the periodic magnetic activity of the system. In addition, the abrupt period reduction may be caused by abrupt mass transfer. If the orbit cycle of YY CrB is indeed prolonged for a long time, it will probably evolve into a fast rotating single star.2 due to the internal and external critical Loche contraction, and the orbit periodic study of two low mass ratio W UMa double stars V728 Her and AH Aur Ming: the orbit cycle of the V728 Her continues to grow, while the AH Aur's orbital period continuously attenuates. Their constant orbital cycle changes suggest that the two stars in these binary stars are experiencing rapid mass transfer. According to the binary star and theory, the V728 Her and the AH Aur are finally available in conjunction with the observations of the blue discrete star and the low mass ratio of the two stars. We can evolve into a fast rotating single star.3 such as the blue discrete star or FK Com. Based on the CCD measurement of V508 Oph, we have determined six new light moments, and found that it has an obvious asymmetric light curve. At the same time, our photometry shows that it is a shallow connection of a mass ratio of Q? 0.552 and a W UMa type of F? 15.4%. Double stars, asymmetric light curves should be caused by hot spots on the surface of the sub star. In addition, the orbit periodic study of V508 Oph shows that its orbit cycle is experiencing a multiple complex change behavior: continuous periodic decay and periodic periodic variation. Multiple periodic changes mean that V508 Oph can be used. The existence of periodic magnetic activity, the material transfer between the two substars and the third celestial.4 around its rotation, we found that V737 Per is a light connected binary star of a W subtype by the first photometric study of the V737 Per, and the observed asymmetric light curve may be caused by the active cold sunspot on the surface of the substar. In addition, we have made the first confirmation. At present, since the available optical minimum time data is only covered in a short time range and does not show any change trend, we can not infer that there is any possible periodic change at present, and the determination of its evolution state also requires a long and deep observation of.5, It is found that the orbital period of shallow connected binary star YY Eri has a long period of orbital periodic growth and a small amplitude periodic change. The long-term periodic growth may be caused by mass transfer from small mass to mass star, and periodic periodic changes can be attributed to the light time orbit effect of third celestial bodies. Periodic magnetic activity. From the analysis of long-period photometric variation, it can be seen that periodic periodic variation is probably caused by periodic magnetic activity.
【学位授予单位】：湘潭大学
【学位级别】：博士
【学位授予年份】：2016
【分类号】：P153
，
本文编号：2175099
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