激变变星及相关天体的H_α与近红外电离钙三重线的光谱分析

给出了1997年4月15日至17日在北京天文台用2．16m望远镜卡焦光谱仪观测获得的6颗激变变星（ABBoo;UXUMa,TCrBAHHer,ZCam和V426Oph）及3颗相关天体（UMa3,EGUMa和Leo3）的CCD光谱,并同时拍摄了5颗晚型星（3Dra,Vir,Leo,34Boo和36Corn）的CCD光谱,作为晚型星参考谱．测量了观测样本星的Hα和近红外CaII的三重线（8498,8542和8662）的等值宽度（EW）,谱线半极大全宽（FWHM）和现向速度（Vr）,并分析了这些星的活动性．     

激变变星及相关天体的Hα与近红外电离钙三重线的光谱分析

给出了１９９７年４月１５日至１７日在北京天台用２．１６ｍ望远镜卡焦光谱仪观测获得的６颗激变变星（ＡＢ Ｂｏｏ,ＵＸ ＵＭａ,Ｔ ＣｒＢ,ＡＨ Ｈｅｒ,Ｚ Ｃａｍ和Ｖ４２６ Ｏｐｈ）及３颗相关天体（ＵＭａ３,ＥＧ ＵＭａ和Ｌｅｏ３）的ＣＣＤ光谱,并同时拍摄了５颗晚型星（３Ｄｒａ,ｖ Ｖｉｒ,ψＬｅｏ,３４Ｂｏｏ和３６Ｃｏｍ）的ＣＣＤ光谱,作为晚型星参考谱,测量了观测样本星的Ｈα和近红外ＣａⅡ的三重     

短周期激变变星周期分布的新统计

我们对周期小于周期分布空缺段的激变变星，重新进行了周期分布统计，使用了比Ｗａｒｎｅｒ等人更多，更新的资料，统计中发现一个ＡＭＨｅｒ型ＣＶｓ：ＧＲＵＶ１偏离了Ｗａｒｎｅｒ等人的统计结果，我们给出了ＣＶＳ新的周期分布图和相应于此分布的随机概率。虽然结果与Ｗａｒｎｅｒ等人的不同，但周期分布同磁场仍呈现一定的相关性，磁激变变星与非磁激变变星同样显示出成团趋势。     

20个激变变星或相关天体的分光证认

在２０个研究得很少的激变变星或者曾经被分类为激变变星的相关天体的光谱中,１３个被证实为属于激变变星（６５％）,另外７个似乎应该被排除（表１第８列）,不像其他研究者那样,仅给出非激变变星或热天体,还以更强的证据和更多的光谱特征征认出１个ＤＡ型白矮星,４个双星系统及其子星的光谱型。新的光谱资料不支持ＦＹ Ｐｅｒ的Ｈｅｒｂｉｇ Ａｅ／Ｂｅ分类,它是一个激变变星。对于ＰＧ１７１２＋４９３,不仅给出星和云的     

短周期激变变星周期分布的新统计

我们对周期小于周期分布空缺段的激变变星(CVs),重新进行了周期分布统计,使用了比Warner等人更多、更新的资料.统计中发现一个AM Her型CVs:GRU V1偏离了Warner等人的统计结果.我们给出了CVs 新的周期分布图和相应于此分布的随机概率.虽然结果与Warner等人的不同,但周期分布同磁场仍呈现一定的相关性,磁激变变星(MCVs)与非磁激变变星(NMCVS)同样显示出成团趋势.     

双星统计演化及激变变星的形成

介绍了双得统计演化的方法和手段,并对激变星的形成进行了Monte-Carlo模拟,模拟显示,激变变星的诞生度、白矮子星质量分布、轨道周期分布的理论结果与观测结果保持一致。另外,还研究了激变变星的形成与模型参量之间的关系,这些参量包括公共包层抛射效率、双星初始质量比分布、年龄、金融丰度等。     

激变变星的辐射模型和多色测光的对比研究

基于黑体模型，本文对激变变星各成分的辐射作了定量的分析，并与观测作了比较。结果表明，简化模型与大多数观测拟合得较好。通过这个模型，我们可以大致看出激变变星不同成分在不同的波段对辐射贡献的相对比例，同时也为我们以前的统计结果给出了一些理论依据。     

激变变星0623＋71的光谱研究

本文提出了激变变星０６２３十７１的４个时间分辨光谱，覆盖轨道周期的７３％．其中的３个谱清楚地显示了各种光谱特征随轨道运动的变化，在流量、能谱以及谱线轮廓方面的这种变化正是对一个倾角不太大的激变变星所期望的．然而另一个曝光对分钟的谱，流量和视向速度与预期的相比都太大，很难加以解释，可能它是一次象ＡＥＡｑｒ中观测到的跃发事件．     

δScuti型变星的观测与模型(英文)

本文报告了δScuti型变星V6 5 0Tau的测光研究结果并讨论了这类变星振幅的变化。根据Arets2 0 0 0的综述“通过谱线变化做模式证认” ,介绍了光谱观测研究δScuti型变星的方法。最后介绍了熊大闰和邓李才的理论模型及δScuti型变星理论的脉动不稳定带     

Two Cataclysmic Variables Identified from ROSAT Bright Sources

This paper presents the results of optical spectroscopic observations of two ROSAT bright sources, 1RXS J020928.9 283243 and 1RXS J042332.8 745300. The low-dispersion spectra suggest the cataclysmic variable classification for the two objects.Further photometric observations are expected to reveal the variable features and to confirm the classifications.     

Cataclysmic variable evolution: AM Her binaries and the period gap

AM Her variables – synchronized magnetic cataclysmic variables (CVs) – exhibit a different period distribution from other CVs across the period gap. We show that non-AM Her systems may infiltrate the longer-period end of the period gap if they are metal-deficient, but that the position and width of the gap in orbital period are otherwise insensitive to other binary parameters (except for the normalization of the braking rate). In AM Her binaries, magnetic braking is reduced as the wind from the secondary star may be trapped within the magnetosphere of the white dwarf primary. This reduced braking fills the period gap from its short-period end as the dipole magnetic moment of the white dwarf increases. The consistency of these models with the observed distribution of CVs, of both AM Her and non-AM Her type, provides compelling evidence supporting magnetic braking as the agent of angular momentum loss among long-period CVs, and its disruption as the explanation of the  2–3 h  period gap among non-magnetic CVs.     

激变变星中的快速光变

文中综述了激变变星中快速光变的研究进展，讨论了闪变，相干振荡和准周期振荡的观测特征和可能的产生机制。     

激变变星3种周期振荡现象 的观测研究进展

激变变星(Cataclysmic Variables, CV)的典型特性是其存在3种周期振荡现象,周期振荡指准周期性的光度快速变化.按光变时标由短到长, CV的周期振荡可分为矮新星振荡、长周期矮新星振荡和准周期振荡.对3种不同振荡在观测上的特征以及在不同亚型CV中的表现进行了介绍,并阐述了可能产生3种周期振荡的物理机制.这些振荡现象为人们研究白矮星的吸积和几何提供了丰富的信息和线索.     

An analysis of early spectroscopic observations and the light curve of the nova V1663 Aql (Nova Aql 2005)

I report the results of a spectroscopic follow‐up of the nova V1663 Aql performed at the Loiano telescope. The emission lines in the spectra have been identified to study the early evolution. The spectra measured some weeks after the maximum show Balmer lines, several Fe multiplets and low ionization lines. The presence of Fe multiplets confirms the original classification of V1663 Aql as a Fe II nova. I have built the light curve using the observations of IAU circulars, VSNET, AFOEV, ASAS databases to estimate the parameters of the nova: time and magnitude of maximum, and the decline rates by two or three magnitudes. The parameters have been used to deduce a distance of V1663 Aql in the range 7.3÷11.3 kpc. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

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.     

The spectroscopic evolution of V2467 Cyg (Nova Cygni 2007) in the first months after the outburst

We present the spectroscopy of nova V2467 Cyg acquired at the Loiano Observatory, Italy, during the first six months after the outburst. We have used the optical spectroscopy to study the physical properties of the ejected material and the photometry to estimate the nova distance. V2467 Cyg is a fast nova, with decline rates by two or three magnitudes of 7.6 and 14.6 days respectively. The light curve exhibited oscillations during the transition stage. The nova achieved an absolute magnitude at maximum in the range –8.5… –9.1. The distance is in the range 2.6… 3.6 kpc. V2467 Cyg showed an early appearance of forbidden lines during the transition stage. Its evolution is similar to the behavior of V1494 Aql (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)