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a cataclysmic variable
相关语句
  激变变星
     Discovery of X-ray Selected AGNs, a White Dwarf and a Cataclysmic Variable
     新发现的X射线选活动星系核、白矮星和激变变星
短句来源
  相似匹配句对
     P.A.
     P. A.
短句来源
     -a!
     的渐近性质,得出如下结论:limb→a!
短句来源
     ON THE CATACLYSMIC METALLOGENESIS
     灾变成矿论
短句来源
     On Selection of the Variable
     关于自变量的选择
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     Cataclysmic Variables
     激变变星
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  a cataclysmic variable
In several respects, W Ser resembles an upscale version of a cataclysmic variable binary system.
      
Results of detailed computer simulations of mass loss from a cataclysmic variable secondary are presented.
      
We consider the possibility that carbon, in the form of the allotrope carbyne, might form in the atmosphere of the white dwarf in a cataclysmic variable system, and be expelled from the system by radiation pressure.
      
Many simplifications to the general model of the nature of a cataclysmic variable are needed to make the system numerically tractable.
      
We describe a method for imaging the accretion disc of a Cataclysmic Variable star.
      
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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。

We have studied 4 time-resolved spectra of the cataclysmic variable 0623+71,covering 73% of the orbit period. Three spectra of them show the variations in fluxes,their distributions and line profiles with the orbital motion, which are expected for a cataclysmic variable having. the inclination not to be very large. For another spectrum with exposure time of 20 minutes, its fluxes and radial velocities are far from the expectation. It is difficult to be explained. It may be something like the flares observed...

We have studied 4 time-resolved spectra of the cataclysmic variable 0623+71,covering 73% of the orbit period. Three spectra of them show the variations in fluxes,their distributions and line profiles with the orbital motion, which are expected for a cataclysmic variable having. the inclination not to be very large. For another spectrum with exposure time of 20 minutes, its fluxes and radial velocities are far from the expectation. It is difficult to be explained. It may be something like the flares observed in AE Aqr.

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.

A set of testing observations were carried out to identify ROSAT sources from PSPC pointing observations and the all sky survey between April 1995 to October 1996. The purpose was to find criteria for searching bright low redshift quasars. As the results of these testing observations, 73 quasars, 27 Seyferts, 1 BL Lac candidate, 1 white dwarf and 1 cataclysmic variable were discovered. The AGNs are not in the AGN catalogue of Veron Cetty and Veron 1995. The optical identifications, measurement...

A set of testing observations were carried out to identify ROSAT sources from PSPC pointing observations and the all sky survey between April 1995 to October 1996. The purpose was to find criteria for searching bright low redshift quasars. As the results of these testing observations, 73 quasars, 27 Seyferts, 1 BL Lac candidate, 1 white dwarf and 1 cataclysmic variable were discovered. The AGNs are not in the AGN catalogue of Veron Cetty and Veron 1995. The optical identifications, measurement of optical positions and E magnitudes were based on the Digital Sky Survey. The spectra were obtained with the 2.16 meter telescope at the Xinglong Station of Beijing Astronomical Observatory. The resolution of the spectra is 9.5?/pixel for the OMR spectrograph and 4.7?/pixel for the Universal spectrogragh. The detector is TEK 1024 CCD. Wavelength and flux calibrations were done with IRAF package. The newly discovered AGNs, white dwarf and cataclysmic variable are list in Table 1 4. The spectra of a quasar, a Seyfert galaxy, a BL Lac candidate, a white dwarf and a cataclysmic variable are shown in Fig. 1 (a e). The spectra of all the sources are available to anyone who is interested in them.

为了研究ROSATX射线选亮近类星体巡天的选择判据 ,从 1 995年 4月至 1 996年 1 0月期间 ,利用北京天文台 2 .1 6米望远镜进行了试验观测 ,发现了 73个类星体、2 7个赛弗特星系、1个BLLac候选体、1个白矮星和 1个激变变星

 
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