Stars That Go Hump in the Night: The SU UMa Stars
Stars That Go Hump in the Night: The SU UMa Stars
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夜间出现的星星：SU UMa 星星
DOI：
10.1007/978-94-009-5337-6_14
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发表时间：
1985
期刊：
影响因子：
--
通讯作者：
B. Warner
中科院分区：
文献类型：
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作者：
B. Warner
灾难性变星的总体结构是在1950年代、60年代和70年代通过光度和光谱观测得出的（参见Robinson（1976）和Warner（1976）的评论）。随着从大变星中发现x射线，以及从低质量x射线双星中获得大量数据，人们对理解与这些恒星有关的更奇特的现象一直感兴趣。特别地，矮新星爆发提供了一种研究非稳定状态的接纳环面或盘的方法。爆发矮新星的大量奇特特性，包括快速相干和准周期光变化、软x射线增强、超极大和超驼峰，需要我们尽一切努力去理解，不仅是为了坚持，而且是为了自信地建立它们的高能兄弟x射线新星、吸积中子星和黑洞的模型。
The gross structure underlying the cataclysmic variable stars was worked out in the 1950’s, 60’s and 70’s from photometric and spectroscopic observations (see reviews by Robinson (1976) and Warner (1976)). With the discovery of X-rays from cataclysmic variables, and the wealth of data from low mass X-ray binaries, there has been a continuing interest in understanding the more exotic phenomena associated with these stars. In particular, dwarf nova outbursts provide a means of studying accetion tori or disks in non-steady states. The abundance of curious properties of outbursting dwarf novae, which include rapid coherent and quasi-periodic light variations, soft X-ray enhancements, supermaxima and superhumps, demands every effort of understanding, not onlypersebut also in order to model with confidence their energetic cousins the X-ray novae, and accreting neutron stars and black holes in general.