密近双星子星间的照射吸收对具有椭率子星表面温度的改变

照射吸收引起的子星表面温度不均匀分布是子星包层大气斜压性的原因,同时又会影响到光变曲线的形态,要了解子星包层大气斜 压性形成的详细图景,要计算双星照射吸收对光变曲线的影响,首先要计算出经过照射吸收后双星表面温度的改变,本在最简单的双球模型的基础上,采用椭球－球模型就椭球受球的照射吸收后所改变的表面温度进行了计算。     

不相接双星的相互照射吸收和子星表面温度的变化

本对不相接双星系统的子星间相互照射吸收进行了计算,从理论上得到子星的表面温度分布情况,对已知基本参数的３３个晚型双星系统中的反映了星等温面和等势面偏离程度的量进行了统计,结果表明,冷子星上等温面向和等热面的偏离程度普遍较热子星的要大。该结果支持了ＺｈｏｕＬｅｕｎｇ所提出了用气旋和反气旋来解释恒星黑子和太阳黑子巨大差别的可能性,本还考虑了临边昏暗效应在晚型双星系统中对子星之间相互照射吸收的影响。     

小质量密近双星Case A演化和几乎相接双星的形成

计算了总质量为3.9M,具有不同初始质比和两子星间距的一组模型在总质量、总角动量守恒假设下的Case A演化,以探求Case A演化与几乎相接双星(NCS)可能的联系.结果表明确实存在经过Case A质量交流演化为NCS系统的途径。并且这样形成的NCS系统其随后的演化有两种前景:一种随即演化为相接系统;另一种则经由慢速质量交流成为较稳定的半接或不接系统.但能够演化为NCS状态的初始模型范围极为狭窄,本文大致确定了它们的初始质比、子星间距等参量范围. 结合模型计算结果,对已知29个NCS系统作了统计研究,结果表明NCS系统与相接双星在演化上有很密切的联系.     

RS CVn型密近双星系统的红外辐射

本文给出了41个RS CVn型密近双星系统的J,H和K的测光结果和经证认为IRAS点源的40个Rs CVn系统的数据。对那些子星具有光谱分类的系统,我们讨论了它们的红外色余,发现只有少数系统具有红外色余。在近红外区有UX Ari,Z Her和HR 1099;在12μm处为SZ Psc。对那些具有确切的12、25μm流量并作了K星等测量的系统,我们讨论了他们在logf_(2.2)/f_(12)和logf_(25)/f_(12)的双色图上的位置。大多数RS CVn系统都在黑体线的附近。这一些结论却和P.Biermann和D.Hall所指出的红外色余是RS CVn型密近双星的一般特性所不相符合。对一些红外辐射有差异的天体应进一步研究。     

密近双星的测量光研究

本文对密近双星中由食、反射效应、引力昏暗效应和临边昏暗放应等引起的标准光变和由子星脉动、黑子、耀斑和热斑等引起的测光畸变以近及相接双星和相接双星光变曲线的不对称性和相接双星光变曲线随时间的变化等进行了详细的综合和讨论。     

密近双星自转的测量和研究（Ⅰ）观测和处理结果

用相同的仪器条件在美国ＫｉｔｔＰｅａｋ国立天文台观测了一批密近双星，并用两种方法得出其自转速度，最后给出了７５个双星系统的９９个子星的自转速度，其中５４个子星是首次进行自转测量。这批高精度的自转值为研究双星的同步性和检验各种同步机制提供了可靠的观测资料。     

密近双星自转的测量和研究（V）轨道圆化

作为密近双星自转测量和研究的系列章之一，本从轨道圆化的角度讨论了Ｚａｈｎ的动力学潮汐机制粘滞理论、Ｔａｓｓｏｕｌ的纯流体动力学理论与实测数据的简便程度，对前前中的２９个不相接双星系统，均分别计算了出以上理论所预测匠轨道沦时标，分析比较了各系统的理论圆化时标与它的年龄及轨道圆化和蔼间的关系，结果表明：动力学潮汐、粘滞理论的计算结果出比纯流体动力学机制的预期更符合实测数据，但与（ＩＶ）的结果相     

密近双星自转的测量和研究（III）同步性的统计性质

我们对前（Ｉ）和（Ⅱ）的实测和计算结果进行了统计分析，讨论了自转同步与相对半径，轨道周期间的关系，结果表明，几乎所有ｒ〉０．１８的不相接双星系统子星都是同步的，而ｒ〈０．１０的子星均处于非同步自转，在相接，半相接双星系统中，同步性与相对半径ｒ也有很好的相关性，但由于子星间物质交流的影响，它们的同步性临界相对半径的０．２１，大于不相接双星系统的０．１８。     

密近双星的演化链

本文对密近双星定化研究的历史和现状作了简要的回顾和概括。从观没和理论计算等不同角度讨论了判断密近双星演化阶段的主要方法。在磊量观测资料的基础上得到了不同类型密近双星演化阶段的主要方法。在大量观测资料的基础上得到了不同类型密近双星的性质和演化阶段。在总结前人工作的基础上,提出了密近双星演化链研究中有毛待进一步研究的问题。给出了知事周期食双星ＡＰ Ｐｕｒ的Ｂ、Ｖ两色光电测光资料。该双星的光变曲线是不对     

A Possible Explanation of the O‘Connell Effect in Close Binary Stars

A theoretical model for explaining the O‘Connell effect of close binary stars is given based on the hypothesis that the circumstellar material of a binary system is captured by its components.The results inferred form the model suggest that late-type and /or short-period binaries can easily produce obvious O‘Connell effect and that the occurrence of O‘Connell effect has no relation with the type of binaries,These conclusions are in agreement with the observed results.The observed O‘Connell effects of six binary systems are examined by the model.For three W-subtype W UMa binaries(YY Eri,BX Per and SW Lac).the densities of the materials captured by the two components are assumed to be equal,and the calculated O‘Connell effect is found to be almost equal to the observed effect.For three A-subtype W UMa systems(CN And,FG Hya and AU Ser),the two densities are assumed to be different,and are calculated separately.The calculated O‘Connell effect turns out to agree better with the observed effect than that was formerly obtained.     

Asynchronous Rotation of a Massive Star in Close Binary Systems

Astrophysics - The problem of asynchronous rotation of massive stars in close binary systems is investigated in this paper. A massive star with twice the sun’s mass, a convective core, and an...     

Research on Periodicity of Single Sector Variable Star of TESS Space Satellite

The short exposure and high precision photometry of TESS (Transiting Exoplanet Survey Satellite) space satellite provide good data for distinguishing variable stars and searching planets. In this paper, a series of methods, such as periodic spectrum and phase folding, are used to analyze 19995 target sources with high-quality variable data in TESS sector 21, and these sources are classified. A total of 4624 variable stars are obtained, including 322 binary stars, 470 pulsating variable stars, and 37 planetary transients. A total of 625 variable sources were cross matched with VSX (The International Variable Star Index). Among them, 131 were eclipsing binary systems and 31 were pulsating variables, whose periods are obtained by periodic spectrum. The other 59 variable stars have flare phenomena, and 8 stars have transiting planets, whose rotation periods are also obtained through the periodic spectrum. The feasibility of the analysis of variable stars by TESS space satellite data is verified. By comparing the period results obtained by TESS space satellite sector 21 with the variable star period provided by VSX variable star table, we found that the periods of most variable stars are consistent with those in this paper, and a few of them need to be corrected. Finally, the verified and corrected variable star tables are provided in this paper.     

估算有中子星作伴星的黑洞质量

在本文中，我们讨论了由中子星和黑洞构成的密近双星系统的引力效应。首先，我们清楚地解释了引力辐射存在引起的轨道圆化，并估算了圆化的时间尺度。求解了围绕史瓦西黑洞作圆轨道运动的矢量进动方程，得到了一个精确解。由进动周期和中心黑洞的质量的关系，我们得到了估算中子星伴随的黑洞质量的方法。随后我们讨论了以中子星脉冲信号随自旋进动变化来寻找黑洞的方法。     

Orbit of an Astrometric Binary System

We present a new method to solve the problem of initial orbit determination of any binary system. This method is mainly based on the material available for an observer, for example relative positions at a given time of the couple in the “plane of sky”, namely the tangent plane to the celestial sphere at the position of the primary component. The problem of orbit determination is solved by splitting in successive stages in order to decorrelate the parameters of each other as much as possible. On one hand, the geometric problem is solved using the first Kepler’s law from a single observing run and, on the other hand, dynamical parameters are then inferred from the fit of the Kepler’s equation. At last, the final stage consists in determining the main physical parameters involved in the secular evolution of the system, that is the spin axis and the J₂ parameter of the primary if we assume that it is a quasi-spherical body. As a matter of fact there is no need to make too restrictive initial assumptions (such as circular orbit or zero eccentricity) and initial guesses of parameters required by a non-linear least-squares Levenberg–Marquardt algorithm are finally obtained after each stage. Such a protocol is very useful to study systems like binary asteroids for which all of the parameters should be considered a priori as unknowns. As an example of application, we used our method to estimate the set of the Pluto–Charon system parameters from observations collected in the literature since 1980.     

Production of Heavy Elements during the Explosion of a Low-Mass Neutron Star in a Close Binary

Astronomy Letters - The nucleosynthesis of heavy elements in the scenario for the evolution of a close binary of neutron stars differing greatly in mass is considered. In contrast to the scenario...     

双星多方模型的形状及其对同步子星轨道要素的摄动影响

研究了双星多方模型的形状对同步子星轨道要素的摄动影响。假定两子星在同一轨道面上运动，推出了主星对伴星的轨道要素的摄动量。理论结果表明：双星多方模型对轨道半长轴和偏心率只有周期项摄动，无长期摄动，但对近星点和历元平近点角除有周期摄动外还有长期摄动效应。文中将理论结果应用于同步双星βＰｅｒ（大陵五双星）的计算上。除计算了两个子星的形状（椭率）外对同步子星的轨道要素变化的周期项振幅和长期项的效应做了数值计算