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     

Elemental abundances for Nova LMC 1990#1

We present our analysis of the UV spectra of the fast ONeMg Nova LMC 1990#1. Observations with the IUE began on 1990 January 18 and continued through to 1990 March 15. We have analysed these spectra, and determined line fluxes and physical parameters as a function of time. Using both He  ii lines and the Balmer decrement, we find the reddening for the nova to be E ( B − V )≃0.22. Using the photoionization code cloudy 90.03b and the minimization routine minuit , we derive elemental abundances for the ejecta. We find the following abundances, relative to solar material: He=1, C=8, N=109, O=20, Ne=62, Mg=16, Al=257 and Si=41. These results are based on independent fits to different data sets acquired three weeks apart. These abundances are extremely similar to those found for V693 Corona Austrinae 1981. Given the position of V693 CrA in the Galaxy and the range of distances found for it, the similar abundances imply that the V693 CrA outburst took place on an older population white dwarf. The high N/O ratio implies an outburst on a massive white dwarf.     

吸积盘边缘的质量和角动量损失与激变双星的演化

本文绘出了计算吸积盘边缘物质和角动量损失，以及它们对激变双星演化影响的理论模型.计算结果表明，紫外天文卫星（IUE）观测到的高速物质流是来源于吸积盘边缘，吸积盘边缘的角动量损失可以成为周期大于3小时的激变双星演化的物理机制．     

Zum optischen Langzeitverhalten von AM Herculis I. Das Beobachtungsmaterial,die Langzeitlichtkurve und der bahninduzierte Lichtwechsel

For the variable binary AM Herculis, which is the proto-type of a subgroup of cataclysmic stars, results from the study of long-term behaviour are given. The following part of the publication concerns the observation series, the long-term light curve and the orbital light changes. On the base of 1275 photographic observations in B, V and U, most of B, covering the time interval between the years 1982 and 1991 new statements can be made about the common photometric behaviour of the star, its low and high states and the mutual correlations between them, the individual influences of the orbital light changes superimposed to the total brighhtness and last but not least about the colour behaviour of the star within these individual occurrences and the whole time interval, which is object of the second part of this study.     

Doppler tomography of cataclysmic variables

The study of cataclysmic variables (CVs), and in particular of the evolution of their accretion discs throughout their different brightness states, has benefited largely from the use of indirect imaging techniques. I report on the latest results obtained from Doppler tomography of CVs concentrating mainly on results published since the 2000 Astrotomography meeting in Brussels. Emphasis is given to the spiral structures found in the accretion discs of some CVs, to the evolution of these structures throughout quiescence and outburst, and to our search for them in more systems. (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)