早型半接食双星猎户座UW的光电测光研究

本文给出UW Ori的首次光电测光结果及新的历元公式。应用Wilson-Devinney综合光变曲线方法得到了初步测光解，结果表明此星是一早型几乎相接的大质量半接双星，质比m2/m1＝0．513,小质量子星临界等位面。由结果的分析指出如大质量子星为零龄主序星，则小质量子星已离开零龄主序。由极小时刻的O－C分析表明周期可能有增长趋势。     

Be／X射线双星UBV光电测光的预备性观测

为研究Be/X射线双星的光度变化,正利用北京天文台60cm望远镜进行UBV光电测光。本文叙述一年来的观测。并结合观测结果对观测和归算方法作了若干讨论,我们主要采用较差测光附加标准星观测以便转换到标准系统。消光计算时考虑零点漂移和可能与大气质量平方的线性关系:m-m_0=k′X k″c k_2X~2 k_tt q。标准系统与观测系统的星等和色指数采用线性关系转换。     

恒星光电测光观数据的处理

简要地阐述了恒星光电测光工作中的常规数据处理方法及应该注意的一些问题。对食双星电测光这一领域的观测数据处理进行了概述,给出了ＢＶ双色光电测光观测数据处理软件包的编程思想及具体实现。最后介绍了这个软件包的使用情况和结果。     

食双星V375 Cas的光电测光研究

本文给出了首次食双星V375 Cas的BV两色光电测光资料和新的历元,并用Wilson-Devinney综合光变曲线方法取得测光解。结果表明:V375 Cas是一个类似RZ Dra的早型半相接双星系统,小质量子星充满了临界等位面,而大质量子星几乎充满了临界等位面,此星对于了解早型密近双星的演化是很有意义的。     

UBV光电测光系统的转换方程和精度比较

根据对鬼星团中Ｊｏｈｎｓｏｎ测光标准星的观测，我们研究了北京天文台６０ｃｍ望远镜直流光电光度计ＵＢＶ测光系统的转换方程．应用该方程推算了对三颗变星观测得到的ＵＢＶ星等，讨论了所得光变曲线的精度，并与较差方法所得结果进行了比较     

盾牌座δ型变星金牛座θ~2的新光电测光

本文给出在北京天文台兴隆观测站获得的盾牌座δ型变星金牛座θ~2的新光电测光资料,它们是新近开展的一次多台站国际联合观测的一部分。以前得到的四频率解(文[1])与新资料符合得极好。单次测量的残差约±0.003星等。     

UBV photometry of the WR binary CQ Cephei

Photoelectric observations of the WR binary CQ Cephei (WN6+O9) are presented. the depths of the eclipses in the light curves are best represented by an inclination of the orbit i = (68°.8±0.6) and the width of the very asymmetric eclipse curves can be represented by only an overcontact configuration (Ω₁ = Ω₂ = 3.65 ± 0.05, and f = 27%). Simultaneous solution of the light and radial velocity curves strongly supports CQ Cep's membership of the Cep OB1 association. By considering this membership we obtained absolute dimensions of the system, which lead to a consistent physical model for CQ Cephei. The more luminous WR primary turns out to be the hotter but slightly less massive component: M_WR = 20.8 M⊙, R_WR = 8.2R⊙, T_eff(WR) = 43600 K, and M_o = 21.4 M⊙, R_o = 8.3 R⊙, T_eff(O) = 37000 K.     

恒星光电测光观测数据的处理

简要地阐述了恒星光电测光工作中的常规数据处理方法及应该注意的一些问题。对食双星光电测光这一领域的观测数据处理进行了概述,给出了ＢＶ双色光电测光观测数据处理软件包的编程思想及具体实现。最后介绍了这个软件包的使用情况和结果。     

A comprehensive photometric study of the marginal-contact binary BE Cephei

New photometry for the eclipsing binary BE Cephei was performed from 2008 to 2011. The light-curve synthesis indicates that it is a marginal-contact binary with a mass ratio of q = 2.340(±0.009) and a degree of contact of f = 6.9%(±2.3%). From the O − C curve, it is discovered that the orbital period changes show a sinusoidal curve superimposed on a downward parabola. The period and semi-amplitude of the cyclic variation are P_mod = 59.26(±0.52) yr and A = 0.^d0067(±0.^d0010), which may be possibly attributed to light-time effect via the presence of an unseen third body. The long-term period decreases at a rate of dP/dt = −4.84(±0.31) × 10⁻⁸ d yr⁻¹, which may result from mass transfer from the more massive component to the less massive one, accompanied by angular momentum loss. With the period decreasing, the degree of contact will increase. Finally, the marginal-contact binary BE Cep may be evolving into a deep-contact configuration.     

Photometry of the Cataclysmic Variables V1159 Ori and BZ UMa

V1159 Ori is an ER UMa sub-type cataclysmic variable belonging to the SU UMa type, and the controversial BZ UMa lies between the U Gem type and the WZ Sge type, but it possesses also the periodicity characteristics of SU UMa. We have made photometric observations of these two cataclysmic variables with the 1m RCC optical telescope in Yunnan Astronomical Observatory from Feb. 24th to 25th, 2008. The obtained light curves of V1159 Ori exhibit superhumps in the descending stage of a normal outburst, this provides an observational evidence for the universal existence of superhumps in ER UMa-type stars. During our observations BZ UMa was at the maximum of an outburst, but no evident superhump period was detected. The previous observations made by AAVSO (American Association of Variable Star Observers) also have never found any definite superhump. This demonstrates that BZ UMa probably is not a SU UMa-type variable. According to the range of its magnitude variations, BZ UMa is closer to WZ Sge.     

Hα Photometry of Two Contact Binaries

We carried out optical and Hα photometry of two contact binaries (V861 Herculis, EQ Tauri). The light curve modeling revealed stellar spots in both contact systems and strong Hα excess in the position of the observed stellar spots. A correlation was found between the V−R and R−H_α colour indices of V861 Her.     

Cyclic period changes and the light-time effect in eclipsing binaries: A low-mass companion around the system VV Ursae Majoris

In this article, a period analysis of the late-type eclipsing binary VV UMa is presented. This work is based on the periodic variation of eclipse timings of the VV UMa binary. We determined the orbital properties and mass of a third orbiting body in the system by analyzing the light-travel time effect. The O−C diagram constructed for all available minima times of VV UMa exhibits a cyclic character superimposed on a linear variation. This variation includes three maxima and two minima within approximately 28,240 orbital periods of the system, which can be explained as the light-travel time effect (LITE) because of an unseen third body in a triple system that causes variations of the eclipse arrival times. New parameter values of the light-time travel effect because of the third body were computed with a period of 23.22 ± 0.17 years in the system. The cyclic-variation analysis produces a value of 0.0139 day as the semi-amplitude of the light-travel time effect and 0.35 as the orbital eccentricity of the third body. The mass of the third body that orbits the eclipsing binary stars is 0.787 ± 0.02 M_⊙, and the semi-major axis of its orbit is 10.75 AU.     

爆后新星武仙V 533的光度研究

老新星武仙V533(V533Her=武仙1963年新星)是一颗光度变化极其复杂的天体。本文给出了我们用双筒天体照相仪于1980年6月至1982年11月间对其所做的照相观测结果。从所得结果可以看到:(1)该星亮度在此期间已基本恢复到其爆前的宁静期亮度;(2)高时频观测指出V533 Her具有时标为小时级,变幅Δm～0.2~m的小幅度光变;(3)在此期间其亮度有上升趋势,上升幅度～1.5等。本文还讨论了V533 Her在爆发前后的光度变化情况,通过分析指出新星在爆发前可能有可觉察的光度变化。     

The CCD photometric study of the newly identified RS CVn binary star V1034 Hercules

This paper presents a new CCD Bessell VR_cI_c light curves and photometric analysis of the newly discovered RS CVn type eclipsing binary star V1034 Her. The light curves were obtained at the Çanakkale Onsekiz Mart University Observatory in 2006. Variations of the orbital period of the system were firstly studied. The (O − C) diagram with a low range of observing time of about 20 years shows an upward parabola, which indicates a secular increase in the orbital period of the system. The light curves are generally those of detached eclipsing binaries; however, there are large asymmetries between maxima. The VR_cI_c light curves were analysed with two different fitting procedures: Wilson–Devinney method supplemented with a Monte Carlo type algorithm and Information Limit Optimization Technique (ILOT). Our general results find V1034 Her. as a well detached system, in which the components are filling 65% of their Roche lobes. Light curve asymmetries of the system are explained in terms of large dark starspots on the primary component. The primary star shows a long-lived spot distribution with active longitudes in the same hemisphere.