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telescope
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  望远镜
    Error Analysis and Correction Technology for Photoelectricity Telescope
    光电望远镜误差分析及补偿技术
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    A DESIGN OF THE CORRECTOR SYSTEM FOR 1.5 METER TELESCOPE
    1.5米望远镜像场改正透镜的设计
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    THE ASTRODOME SERVO SYSTEM OF THE 60 cm TELESCOPE
    60厘米望远镜圆顶随动系统
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    THE KD P MODULATOR IN THE SOLAR MAGNETIC FIELD TELESCOPE
    太阳磁场望远镜中KD~*P电光调制器
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    THE DESIGN OF THE 1.56m ASTROMETRIC TELESCOPE
    1.56米天体测量望远镜设计
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  望远
    Optical Design of Hybrid Reflective/Diffractive Binary Optics Schmidt Telescope
    二元光学反/衍混合Schmidt望远系统光学设计
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    Amend wave-front errors in measurement on the wave-front of large telescope
    大型望远系统波前检测中的波前误差修正
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    A binary optics reflective/diffractive Schmidt telescope was designed using diffractive optical element (BOE) to replace the Schmidt corrector to correct aberrations.
    针对空间光学系统轻型的特点,采用衍射光学元件取代Schmidt校正板来校正系统像差,设计了一个二元光学反/衍混合Schmidt望远系统。
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  天文望远镜
    Stady of Large Sky Area Multi-Object Fiber Spectroscopic Telescope ——Observatory Control System of Level 0
    大天区面积多目标光纤光谱天文望远镜的研究——0级观测控制系统
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    Study of Large Sky Area Multi-object Fiber Spectroscopic Telescope—The Effect of S-H Method on Tiling
    大天区面积多目标光纤光谱天文望远镜的研究——S-H检验对天区覆盖的影响
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    High precision friction drive of large telescope
    大型天文望远镜高精度摩擦传动的研究
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    The Application of Fuzzy-control in Astronomical Telescope Control System
    模糊控制在天文望远镜控制系统中的应用
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    The Application Of DELPHI In The Equatorial Astronomical Telescope Control System
    DELPHI语言在赤道式天文望远镜控制系统中应用
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  “telescope”译为未确定词的双语例句
    Control, Optimization and Experiment of the Feed Tracking System for Large Radio Telescope
    大型射电望远镜馈源指向系统的控制、优化与实验
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    400mm HORIZONTAL SOLAR TELESCOPE AND MULTIPLE SPECTRAL REGION SPECTROGRAPHS
    400毫米水平式太阳望远镜和多波段摄谱仪
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    the Improved Calibration System of the Solar Radio Telescope at 9375 MHz and Its Indoor Control Device
    9375MHz太阳射电望远镜新定标源系统及其室内控制装置
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    A Method of Precisely Adjusting the Polar Axis of an Equatorial Radio Telescope
    一种赤道式射电望远镜极轴的精密校准方法
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    FeI λ 5324.19(?) LINE FORMS IN THE SOLAR MAGNETIC FIELD AND THE THEORETICAL CALIBRATION OF THE SOLAR MAGNETIC FIELD TELESCOPE
    FeIλ5324.19在太阳磁场中的形成和太阳磁场望远镜的理论定标
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  telescope
The effect of cosmic ray shadowing by the Moon is observed by recording the single muon component with the Baksan underground scintillation telescope (BUST).
      
The Tanaka-Enome criterion and solar activity in October-November 2003 as observed by the Large Pulkovo Radio Telescope
      
The observations are made with the Large Pulkovo Radio Telescope (LPRT) in the range 2.7-20 cm, the one-dimensional (E-W) resolution of observations being 1-6 arc min, respectively.
      
Development of the GAMMA-400 gamma-ray telescope to record cosmic gamma rays with energies up to 1 TeV
      
A photomultiplier tube for a NT-200 deep-underwater neutrino telescope
      
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According to the international convention,we have carried out the photographic photometry on the U,B,V system,with the recommended plate-filter combinations:U— Kodak 103a-O+UG2;B—103a-o+GG13 and V—103a-D+GG11.Our telescope is a 15 cm Zeiss astrograph (UV objective).With the data in hand,we cal- culated the effective wave length of the blue combination.(103a-o+GG13)to be 4440A and the yellow combination (103a-D+GG11) 5610A.Both are longer than that of the respective B,V system. When we determine the magnitudes...

According to the international convention,we have carried out the photographic photometry on the U,B,V system,with the recommended plate-filter combinations:U— Kodak 103a-O+UG2;B—103a-o+GG13 and V—103a-D+GG11.Our telescope is a 15 cm Zeiss astrograph (UV objective).With the data in hand,we cal- culated the effective wave length of the blue combination.(103a-o+GG13)to be 4440A and the yellow combination (103a-D+GG11) 5610A.Both are longer than that of the respective B,V system. When we determine the magnitudes of stars from focal images,there are systema- tic differences between ours and the U,B,V system.Since our refractor has larger chromatic aberration in some wave length regions,the system of magnitudes is very sensi- tive to focus change.There exists a range of focus-setting,in which systematic dif- ferences can be eliminated.The range is different in the three combinations.For the combination 103a-D+GG11,the setting is about 2 mm out of focus with a tolerance of±0.2mm.For 103a-O+GG13 the range is rather wide from 1.5mm to far out of focus.For 103a-O+UG2 it is even wider,from about 1.0mm to far out of focus. As the check of the above results we observed four open clusters M44,M45, NGC752,and IC4665.The reddened O-association CygⅥ was also observed with 103a-D+GG11.Within the expected precision of photograpic photometry no sys- tematic errors are found. We measure the plates by a Sartorius Iris photometer.The characteristics of the Iris photometer together with measuring errors are discussed. Besides,we have preliminarily investigated the influence of defective guiding, which,as is found out,can be neglected. Finally,we give four light curves of variable stars (UY Boo,RU Psc,VZ Cnc,and SZ Tau).For SZ Tau we use the combination 103a-O+UG2 and for the others the combination 103a-D+GG11.

本文叙述根据较差测量法,试用柯达103a—D+GG11、103a—O+GG13及103a—O+UG2组合,对本台口径15厘米折光镜进行 U、B、V 系统照相测光.结果表明,前两种组合的有效波长约为5610及4440,比 B、V 系统的长.焦点照相结果,星等与标准值有系统差.这具望远镜消色差在蓝紫波段,当在其他波段测光时,焦距调节对星等测定极为敏感.但存在一个焦距调节范围,在此范围内照相,可以消去系统差.这个范围对三种组合都不同.103a—D+GG11,约在该组合的焦点以外2毫米处,可变范围约±0.2毫米;对103a—O+GG13,从该组合焦外1.5厘米到星象显著变大的焦外;对103a—O+UG2,从该组合焦外约1毫米到星象显著变大的焦外.为校验上述结果,拍摄了疏散星团M45, M45,NGC752和IC4665.用103a—D+GG11还观测了红化 O 星协 CygⅥ.在我们使用这架望远镜进行照相测光工作所要求的精度下,这个方法是可以应用的.我们使用萨尔托累光瞳光度计(Sartorius Iris Photometer)测量底片,讨论了测量方法及误差.此外,还考察了导星不好的初步后果,在我们所要求的精度上没有...

本文叙述根据较差测量法,试用柯达103a—D+GG11、103a—O+GG13及103a—O+UG2组合,对本台口径15厘米折光镜进行 U、B、V 系统照相测光.结果表明,前两种组合的有效波长约为5610及4440,比 B、V 系统的长.焦点照相结果,星等与标准值有系统差.这具望远镜消色差在蓝紫波段,当在其他波段测光时,焦距调节对星等测定极为敏感.但存在一个焦距调节范围,在此范围内照相,可以消去系统差.这个范围对三种组合都不同.103a—D+GG11,约在该组合的焦点以外2毫米处,可变范围约±0.2毫米;对103a—O+GG13,从该组合焦外1.5厘米到星象显著变大的焦外;对103a—O+UG2,从该组合焦外约1毫米到星象显著变大的焦外.为校验上述结果,拍摄了疏散星团M45, M45,NGC752和IC4665.用103a—D+GG11还观测了红化 O 星协 CygⅥ.在我们使用这架望远镜进行照相测光工作所要求的精度下,这个方法是可以应用的.我们使用萨尔托累光瞳光度计(Sartorius Iris Photometer)测量底片,讨论了测量方法及误差.此外,还考察了导星不好的初步后果,在我们所要求的精度上没有发现显著影响.

A zenith-telescope,ZTL-180,has been mounted at the Tientsin International Lati- tude Station in the Summer of 1958. Observations of latitude variations have been made since January 1959.During the first three years 10203 star pairs were observed on 702 nights. The results of the determination of the declination corrections for each group and cach pair and the variations of latitude are given.Preliminary values of the polar mo- tion were calculated with our latitude variations by A.J.Orlov's method.

天津纬度站于1958年夏安装了一架口径180毫米,焦距2340毫米的目视天顶仪.仪器位于北纬39°8′纬线上.1959年1月开始了正式的纬度观测.三年内,在702个晴夜中共得10203个纬度值.本文利用这些观测,定出了所用星对的赤纬改正,求出津站三年间的纬度变化以及周年非极性变化,并利用纬度变化结果按奥洛夫法对地极坐标作出了试算结果.

The photographic photometry of Nova was observed with three colours—ultraviolet, blue and yellow—from February 17 to November 19,1963.The telescope and plate- filter combinations are the same as those described in a previous paper.Some additional explanation of our magnitude systems has been made.Since the magnitudes of the nearby stars are not suitable for comparison,we have to determine it independently by the usual photographic method.The magnitudes of Nova and comparison stars are given. We discussed...

The photographic photometry of Nova was observed with three colours—ultraviolet, blue and yellow—from February 17 to November 19,1963.The telescope and plate- filter combinations are the same as those described in a previous paper.Some additional explanation of our magnitude systems has been made.Since the magnitudes of the nearby stars are not suitable for comparison,we have to determine it independently by the usual photographic method.The magnitudes of Nova and comparison stars are given. We discussed the light curves of Nova with logarithmic curves;it seems feasible. Spectral observations were made with the slit spectrograph used at the Cassegrain focus of the 60-cm reflector of the Purple Mountain Observatory,in the interval between February 21 and August 8,1963.The linear dispersion of the spectrograph is about 153A/mm at Hr.In this paper the characteristics and changes of the spectra have been described,and the expansion velocity of the envelope of the Nova is given. Six microphotometer tracings of spectra,on both the photographic and the visual regions,are illustrated in Figure(4),and in Figure(5)is also shown a tracing of the spectrum of “netrogen flaring”.

1963年紫金山天文台对1963年武仙座新星(NHer 1963)~(++)作了三色(紫外、蓝、黄)照相测光和光谱观测.照相测光从2月17日开始到11月9日为止,用照相方法独立测定了星等,列出了新星和比较星的星等.用对数曲线法讨论了新星光变曲线.光谱观测自2月21日开始至8月8日结束.文中叙述了光谱的特征和变化,列出了壳层膨胀速度的测量结果,以及照相区和目视区的新星光谱描记图各6张,4月24日到25日的“氮闪”光谱描记图一张.

 
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