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矮新星
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  dwarf nova
     Physical Explanation to SU UMa-type Dwarf Nova's Explosion and Super-explosion
     SU UMa-type矮新星爆发和超爆发的物理解释
短句来源
     In this paper the least-squares fit for dwarf nova AB Dra shows that the continuum predicted by the blackbody accretion disk model can roughly fit to the observed IVE data and the smaller deviation may be attributed to an appropriate amount of recombination radiation from optically thin gas or/and black body radiation from the hot spot.
     对矮新星ABDra的最小二乘拟合表明,黑体吸积盘模型预言的连续谱能粗略地拟合该星在爆发期间的IUE观测,较小的偏差可以归因于光学薄气体的复合辐射或/和热斑的黑体辐射。
短句来源
     This article gives the physical explanation to SU Uma-type dwarf nova's explosion and super-explosion.
     本文介绍了SUUMa -type矮新星爆发和超爆发及其物理解释
短句来源
  dwarf novae
     SU UMa-type Dwarf Novae and Research About It
     SU UMa-type矮新星及其研究
短句来源
     SU UMa-type dwarf novae play an important role in understanding the evolution of dwarfnovae. the chara cteristic patterns was shown in the visual light curves of dwarf novae systems combine the light curves from observations,the new characteristic patterns of light curves form observations and the physical source of light curve of cataclysmic variables(accretion discs model of dwarfnova).
     介绍了 SU UMa-type矮新星可见光光变曲线特性 ,综述了近期的观测成果以及激变变星光变的物理根源—— SU UMa-type吸积盘模型及最新的研究成果 ,并介绍了笔者在该领域所做的一些工作 .
短句来源
  “矮新星”译为未确定词的双语例句
     OPTICAL STUDY OF EG CANCRI OUTBURST IN 1996
     对矮新星EG Cancri 1996年爆发的研究
短句来源
     3 candidates are shown to be CVB, which are PG0027 + 260, PG0818 + 513 and PG1030+ 590; 2. One candidate PG1551 +719 is a SU UMa type CV; 3. PG1341-079 is a possible CVB;
     其光变曲线特性表明:PG0027+260,PG0818+513,和PC1030+590为激变食变星,PG1341—079 是一个可能的激变食变星,PG1551+719为SU UM_a型矮新星,此外还有6个天体的光变曲线有激变星特有的闪变特征.
短句来源
     ON THE ACCRETION DISK IN AB DRACONIS
     矮新星AB Dra中的吸积盘模型
短句来源
     The optical light curve of EG Cancri during its outburst in 1996~1997 were presented. It has displayed some brightness fluctuations in the phase of decline.
     给出了矮新星EGCue在1996~1997年爆发期间的光变曲线和光谱。
短句来源
     EG Cancri is a CVs that has large - amplitude outburst (7mag), slow decline from outburst, long intervals between outburst and short period. From above properties, we classify the CVs, EG Cancri, as a WZ Sge type DN is plausible.
     由于EGCnc具有大变幅爆发(≈7mag),缓慢下降,爆发间隔长(19年),极短轨道周期和superhump等特征,我们认为这是一颗较少见的WZSge型矮新星
短句来源
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  相似匹配句对
     nova
     新星
短句来源
     SU UMa-type Dwarf Novae and Research About It
     SU UMa-type新星及其研究
短句来源
     Novae and Supernovae.
     新星和超新星
短句来源
     OPTICAL STUDY OF EG CANCRI OUTBURST IN 1996
     对新星EG Cancri 1996年爆发的研究
短句来源
     Cheng, E.
     Cheng、麻黄E.
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  dwarf nova
Photometric parameters of the dwarf nova SS Cygni in the quiescent state
      
The mean 1983-1996 UBV light curves of the dwarf nova SS Cyg are used to derive the binary parameters in the quiescent state.
      
We interpret optical and IR orbital light curves of the dwarf nova U Gem in its quiescent state in the framework of "hot line" and "hot spot" models.
      
Some related discussion is also given to nova and dwarf nova systems.
      
The similarity in properties of GK Per and BV Cen suggests that the latter may be a classical nova remnant rather than a dwarf nova.
      
更多          
  dwarf novae
Last year its behavior became non-typical for "anti-dwarf novae".
      
Space densities and galacticz-distributions of novae, recurrent novae, dwarf novae and symbiotic stars are newly determined and discussed in the context of earlier determinations.
      
The (B-V) colour variation with respect to the 67 min variation is found to be opposite to those of typical colour variation during hump/superhump activity in other dwarf novae.
      
Far infrared observations of the two possible types of progenitor, R Coronae Borealis-type stars and dwarf novae, would be useful to indicate whether there is any dust around them which would survive a supernova outburst.
      
High Speed Photometry of four eclipsing dwarf novae, z Cha, OY Car, HT Cas and IP Peg, is used to determine the orbital parameters and the masses of the two stars in each system.
      
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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. .3 candidates are shown to be CVB, which are PG0027 + 260, PG0818 + 513 and PG1030+ 590;2. One candidate PG1551 +719 is a SU UMa type CV;3. PG1341-079 is a possible CVB;4. 5 objects show definitely light flickering which is the characteristics of CV;g. The orbital period for PG1030...

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. .3 candidates are shown to be CVB, which are PG0027 + 260, PG0818 + 513 and PG1030+ 590;2. One candidate PG1551 +719 is a SU UMa type CV;3. PG1341-079 is a possible CVB;4. 5 objects show definitely light flickering which is the characteristics of CV;g. The orbital period for PG1030 + 590 is determined from 5 observed minima, as P =3h.2792;6. The variation of the amplitude in flickering for PG1717 + 413 is significant in 2 month time-base line, and is not correlated with the magnitude of the object. It is suggested that the bright spot might be responsible for such phenomena;7. The probability of finding CV by using UVX and emission line technique is about 71%.

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.其光变曲线特性表明:PG0027+260,PG0818+513,和PC1030+590为激变食变星,PG1341—079 是一个可能的激变食变星,PG1551+719为SU UM_a型矮新星,此外还有6个天体的光变曲线有激变星特有的闪变特征.因此PG样本中,激变变星的成功率为79%.PG1030+590的轨道周期为3~h279,PG1717+413的闪变变幅在二个月内有明显变化,它与本身的亮度无明显相关,说明闪变变幅的变化可能是亮斑的局部效应.

In this paper the least-squares fit for dwarf nova AB Dra shows that the continuum predicted by the blackbody accretion disk model can roughly fit to the observed IVE data and the smaller deviation may be attributed to an appropriate amount of recombination radiation from optically thin gas or/and black body radiation from the hot spot.From the fitting we have obtained the reasonable values of some parameters of the disk and the system which it belongs to.

矮新星ABDra的最小二乘拟合表明,黑体吸积盘模型预言的连续谱能粗略地拟合该星在爆发期间的IUE观测,较小的偏差可以归因于光学薄气体的复合辐射或/和热斑的黑体辐射。拟合给出了一组吸积盘参量的合理值。

The optical light curve of EG Cancri during its outburst in 1996~1997 were presented.It has displayed some brightness fluctuations in the phase of decline. Mini - outbursts were detected. Optical spectra obtained during the decline showed it to be a dwarf nova on account of its broad absorption lines superimposed on a blue continuum. Optical spectra near minimum brightness revealed doubled Balmer lines in emission, over broad absorptions, but no HeII4686. An additional heating presented in the last stage of...

The optical light curve of EG Cancri during its outburst in 1996~1997 were presented.It has displayed some brightness fluctuations in the phase of decline. Mini - outbursts were detected. Optical spectra obtained during the decline showed it to be a dwarf nova on account of its broad absorption lines superimposed on a blue continuum. Optical spectra near minimum brightness revealed doubled Balmer lines in emission, over broad absorptions, but no HeII4686. An additional heating presented in the last stage of decline. CCD time - resolved photometry showed a possible orbital period 0. 0575 ±0. 0026 day. Superhumps were observed during outburst by Matsumoto(1996). EG Cancri is a CVs that has large - amplitude outburst (7mag), slow decline from outburst, long intervals between outburst and short period. From above properties, we classify the CVs, EG Cancri, as a WZ Sge type DN is plausible.

给出了矮新星EGCue在1996~1997年爆发期间的光变曲线和光谱。光变曲线显示了它在下降过程中有较大的亮度波动及mini-outburst。光谱从爆发时的蓝吸收谱演化为宁静期有双峰的巴尔末发射线谱。从宁静期的CCD快速测光,得到它的轨道周期为0.0575±0.0026天。Matsumoto[1]观测到了爆发期的superhump。由于EGCnc具有大变幅爆发(≈7mag),缓慢下降,爆发间隔长(19年),极短轨道周期和superhump等特征,我们认为这是一颗较少见的WZSge型矮新星

 
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