W UMa型相接雙星的觀測與研究
發(fā)布時間：2018-08-09 19:36
【摘要】：W UMa型雙星是一類兩子星均充滿或超過其洛希瓣并形成公共對流層的相接雙星系統(tǒng)。它們所具有的啞鈴形結(jié)構(gòu)使得其兩子星極易發(fā)生相互掩食,展現(xiàn)出連續(xù)變化的光變曲線和幾乎相等的兩食深。同時,共享的對流公共包層使得兩子星之間可發(fā)生諸如物質(zhì)與能量的交流和通過外拉格朗日點的物質(zhì)、能量與角動量的損失等復雜的物理現(xiàn)象。獨特的幾何結(jié)構(gòu)與這些復雜的物理過程使得W UMa型相接雙星成為人們普遍關注的一類天體系統(tǒng)。本論文以W UMa型相接雙星為對象,研究了一批樣本星的軌道周期變化行為和部分樣本星的結(jié)構(gòu)特征與演化狀態(tài),得到了如下的一些研究結(jié)果:1、對W UMa型相接雙星YY Cr B的軌道周期研究表明,該系統(tǒng)既有可能正經(jīng)歷連續(xù)的周期衰減,同時伴隨著周期的周期性變化,也有可能在過去的20年里經(jīng)歷了一次陡然的周期減小。長期的周期減小可能是由于從主星到次星的質(zhì)量轉(zhuǎn)移或由恒星風所致的質(zhì)量損失引起的;而周期性的周期改變應該不是由第三天體的光時軌道效應所致,而應歸結(jié)于系統(tǒng)的周期性磁活動;另外,陡然的周期減小可能是因陡然的質(zhì)量轉(zhuǎn)移所致。如果YY CrB的軌道周期確實是長期減小的,那么它將很可能因內(nèi)外臨界洛希瓣收縮而演化成一顆快速旋轉(zhuǎn)單星。2、對兩顆低質(zhì)量比深度相接W UMa型雙星V728 Her和AH Aur的軌道周期研究表明:V728 Her的軌道周期連續(xù)增長,而AH Aur的軌道周期連續(xù)衰減。它們恒定的軌道周期變化暗示著這些雙星中的兩子星正經(jīng)歷快速的質(zhì)量轉(zhuǎn)移。依據(jù)雙星并和理論,并結(jié)合藍離散星和低質(zhì)量比深度相接雙星的觀測特征,V728 Her和AH Aur最終可能演化成諸如藍離散星或FK Com型的快速旋轉(zhuǎn)單星。3、基于V508 Oph的CCD測光觀測,我們確定了六個新的光極小時刻,發(fā)現(xiàn)了它具有明顯不對稱的光變曲線。同時,我們的測光解表明它是一顆質(zhì)量比為q?0.552和相接度為f?15.4%的W UMa型淺度相接雙星,不對稱的光變曲線應該是次星表面存在活動的熱黑子所致。另外,對V508 Oph的軌道周期研究表明它的軌道周期正經(jīng)歷一個多重的復雜變化行為:連續(xù)的周期衰減,同時伴隨著周期性的周期變化。多重的周期變化行為意味著V508 Oph可能存在周期性的磁活動、兩子星間的物質(zhì)轉(zhuǎn)移和圍繞其轉(zhuǎn)動的第三天體。4、通過對V737 Per的首次測光研究,我們發(fā)現(xiàn)V737 Per是一顆W次型的淺度相接雙星,而觀測得到的不對稱光變曲線可能是次星表面活動性冷黑子所致。另外,我們首次確定了其測光質(zhì)量比和相接度。目前,由于可利用的光極小時刻數(shù)據(jù)僅覆蓋了較短的時間范圍且沒有展現(xiàn)出任何的變化趨勢,所以我們當前不能夠推斷其存在任何可能的周期變化行為,而且其演化狀態(tài)的確定還需要長期且深入的觀測。5、發(fā)現(xiàn)淺度相接雙星YY Eri的軌道周期存在長期的軌道周期增長的同時附加了一個小幅度的周期性變化。長期的周期增長可能是從小質(zhì)量次星向大質(zhì)量主星的物質(zhì)轉(zhuǎn)移所致,而周期性的周期變化能夠歸因于第三天體的光時軌道效應或者周期性的磁活動。從長周期的光度變化分析可知,周期性的周期變化很可能是由周期性磁活動所引起。
[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.
【學位授予單位】：湘潭大學
【學位級別】：博士
【學位授予年份】：2016
【分類號】：P153
，
本文編號：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.
【學位授予單位】：湘潭大學
【學位級別】：博士
【學位授予年份】：2016
【分類號】：P153
，
本文編號：2175099
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