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cataclysmic variable
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  激变变星
     The Discovery of Four Cataclysmic Variable Stars in1997 at Beijing Observatory
     北京天文台1997年发现四颗激变变星
短句来源
     THE SPECTROSCOPIC STUDY OF CATACLYSMIC VARIABLE 0623+71
     激变变星0623+71的光谱研究
短句来源
     THE CLEAN METHOD OF SPECTRAL ANALYSIS AND ITS APPLICATION IN ANALYZING THE SHORT PERIOD OSCILLATIONS OF CATACLYSMIC VARIABLE TT ARI
     谱分析的CLEAN方法及其在激变变星TT Ari短周期振荡分析中的应用
短句来源
     This paper presents the observational result of the light curves for 14 PG cataclysmic variable candidates using the, 60/90/180 cm Schmidt Telescope and Thomson 576×384 CCD of Beijing Astronomical Observatory. The main results are:1. .
     我们于1989年用北京天文台兴隆观测站的60/90/180厘米施密特望远镜及Thomson红敏CCD对14个PG候选激变变星进行光度观测.
短句来源
     Su UMa-type dwarf novas belong to cataclysmic variable stars, whose character is magnified explosion, i.e., super-explosion.
     SUUMa -type矮新星属于激变变星 ,其特征是存在扩大了的爆发即超爆发。
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  “cataclysmic variable”译为未确定词的双语例句
     A CCD Light Curve of the Eclipsing Cataclysmic Variable PG0027+260
     激变食变星PG0027+260的CCD光变曲线
短句来源
  相似匹配句对
     THE SPECTROSCOPIC STUDY OF CATACLYSMIC VARIABLE 0623+71
     激变变星0623+71的光谱研究
短句来源
     Cataclysmic Variables
     激变变星
短句来源
     On Selection of the Variable
     关于自变量的选择
短句来源
     On Analysis of Variable
     论变量分析法
短句来源
     ON THE CATACLYSMIC METALLOGENESIS
     灾变成矿论
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  cataclysmic variable
CCD Photometry of the Cataclysmic Variable SW Ursae Majoris at a Late Stage of the 2000 Superoutburst
      
We report the first millimetric detections of the magnetic cataclysmic variable AE Aquarii, accompanied by contemporaneous microwave observations.
      
The spectral shape of the far-UV continuum closely resembles that of a UX UMa type cataclysmic variable.
      
In several respects, W Ser resembles an upscale version of a cataclysmic variable binary system.
      
The cataclysmic variable EX Hydrae has been observed in X-rays with Einstein Observatory.
      
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The cataclysmic variable is a close binary system, in which a low-mass, late-type secondary star fills its Roche lobe and is transferring its mass to a white dwarf primary star. In most of these systems the transferred mass forms an accretion disk around the primary star. Cataclysmic variables are important objects to our understanding accretion processes,evolution of close binaries,and other interesting issues. In the present paper a summary of observational researches on cataclysmic variables is given...

The cataclysmic variable is a close binary system, in which a low-mass, late-type secondary star fills its Roche lobe and is transferring its mass to a white dwarf primary star. In most of these systems the transferred mass forms an accretion disk around the primary star. Cataclysmic variables are important objects to our understanding accretion processes,evolution of close binaries,and other interesting issues. In the present paper a summary of observational researches on cataclysmic variables is given and a few unsolved problems are discussed as well.

激变变星是密近双星系统,包含一颗白矮星主星和一颗晚型星伴星。晚型星伴星充满了其Roche瓣,并向主星转移物质,在主星周围形成一个吸积盘。这类双星对于我们认识吸积过程、密近双星的演化等是相当重要的。本文主要从实测角度综述激变变星研究的现状,并讨论一些尚待解决的问题。

According to its color and spectral features, i.e. (U- B) < - 0.4 mag and strong emission lines in its spectra, PG1030 + 590 was selected as a cataclysmic variable candidate by Green et al. (1982). Observations by Shafter showed that PG1030 + 590 is a single-lined, eclipsing nova-like variable. Since then neither spectroscopic nor photometric observations of this system has been published.We obtained high-speed photometry of PG1030 + 590 in April 1984 and April 1985. From the finding chart given...

According to its color and spectral features, i.e. (U- B) < - 0.4 mag and strong emission lines in its spectra, PG1030 + 590 was selected as a cataclysmic variable candidate by Green et al. (1982). Observations by Shafter showed that PG1030 + 590 is a single-lined, eclipsing nova-like variable. Since then neither spectroscopic nor photometric observations of this system has been published.We obtained high-speed photometry of PG1030 + 590 in April 1984 and April 1985. From the finding chart given by Green et al. two stars were chosen as the comparison stars. Multicolor light curves are presented in Fig. 1. We obtained five eclipses of PG1030 +590. The five mid-eclipse times, plus those obtained by Shafter, yield an ephemeris of PG1030+590.By using the basic model of cataclysmic variables and assuming that the secondary star follows the mass-radius relation for low-mass main sequence stars we have calculated the parameters of PG1030 + 590: M1 = 0.83±0.22M⊙; M2 = 0.35±0.06M⊙;q = M2/M1 - 0.42± 0.05;i = 81°±2°;R2 = 0.37±0.08R⊙; and a = 1.20±0.10R⊙. The size of accretion disk in PG1030 + 590 is calculated by using two methods. The first is to calculate the photometric radius of the disk, which in turn yields the radius of the disk. The second method is to use the relations given by Sulkanen et al. (1981). The two methods give the same result: Rd = 0.32R⊙, which is about 60% the size of the Roche lobe of the primary star.

PG1030+590是最近发现的类新星食变星。我们首先给出该双星系统的高速光电测光结果及U、B、V和R光变曲线。通过利用激变变星的模型对观测结果进行分析,我们求得其物理和几何参数:白矮星子星质量M_1=0.83±0.22M_⊙,晚型星子星质量M_2=0.35±0.06M_⊙,晓型星子星半径R_2=0.37±0.08R_⊙以及轨道倾角i=81°±2°。我们还利用两种不同方法求出围绕白矮星的吸积盘的半径R_d≈0.32R_⊙,并把这个结果与密近双星中吸积盘半径的各理论模型进行了比较。

About 100 compact galactic X-ray sources have been identified optically. Most of them are binaries consisting of compact stars (white dwarfs, neutron stars or black holes). They can be divided into three main categories; (1) with a massive binary companion forming a High Mass X-ray Binary, or HMXB for simplicity, (2) with a low mass late type binary companion, or LMXB, (S) Cataclysmic variable. Here we give a brief introduction to them, putting less emphasis on the later.

已被光学证认的约100个致密X射线源,绝大部分是一颗致密星(白矮星、中子星或黑洞)与另一恒星组成的双星。其中主要有三种类型:(1)伴星为大质量早型星,简称HMXB;(2)伴星为低质量晚型星,即LMXB;(3)激变变星。本文重点简介前两类的基本观测事实及理论模型,也顺便提到后者。

 
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