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photoelectric photometer
相关语句
  光电光度计
     THE PHOTOELECTRIC PHOTOMETER FOR THE 1.56m TELESCOPE OF SHANGHAI OBSERVATORY
     上海天文台1.56米望远镜光电光度计的研制
短句来源
     Cepheid variables CY Aqr and BE Mon were observed at the Purple Mountain Observatory with a photoelectric photometer during December 1959 and the first two months of 1960.The observations of CY Aqr (Table 1) made on four nights provide sufficient data for plotting five complete light curves (Fig.1) of this variable.
     用紫金山天文台的60厘米反光望远镜和1P21光电倍增管所构成的光电光度计,我们在1959年底和1960年初,对 CY Aqr 及 BE Mon 进行了测光观测. 得到 CY Aqr 的五条完整的光变曲线.
短句来源
     A NEW PHOTOELECTRIC PHOTOMETER FOR THE 60cm TELESCOPE OF BEIJING OBSERVATORY
     北京天文台60cm望远镜的新光电光度计
短句来源
     The total luminous flux of the solar corona was measured by a photoelectric photometer with a 3°field during the total solar eclipse of 1997 March 9 at Mohe, Heilongjiang Province.
     在漠河1997年3月9日日全食期间,使用3°测量视场的光电光度计,测量了日冕总光通。
短句来源
     The times of 6 maxima of the ultrashort-period cepheid variable EH Librae were measured in May to June, 1980, and in January, 1981, with a three channel photoncounting high-speed photoelectric photometer.
     我们于1980年5月18、19日及6月15日和1981年1月15日四夜,用高速光电光度计观测了天秤座EHLib,获得6个光度极大时刻。
短句来源
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  “photoelectric photometer”译为未确定词的双语例句
     A PHOTOELECTRIC PHOTOMETER FOR THE OBSERVATION OF OCCULTATION
     掩星观测用的光电光度计
短句来源
     The Photoelectric Photometer Attached to the I M Telescope
     一米望远镜光电光度计
短句来源
     The Integrated Photoelectric Photometer System Used with A Microcomputer
     利用微型机的积分光度计系统
短句来源
     Report on the Test Observation of An Integrated Photoelectric Photometer
     积分光度计系统试观测报告
短句来源
     A Photoelectric Photometer Attached to A 35-cm Telescope
     35厘米望远镜光电光度计
短句来源
  相似匹配句对
     The Photoelectric Photometer Attached to the I M Telescope
     一米望远镜光电光度计
短句来源
     A PHOTOELECTRIC PHOTOMETER FOR THE OBSERVATION OF OCCULTATION
     掩星观测用的光电光度计
短句来源
     Transverse Photoelectric Effect
     横向光电效应(英文)
短句来源
     Photoelectric Reconnassiance for Coast
     沿海光电侦察技术
短句来源
     Photometer for Flashing Light
     瞬态光度计
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  photoelectric photometer
In the spectroscopic data obtained at Norikura, we have detected and confirmed the earlier detection of 5-minute oscillations in photoelectric photometer observations made at Lomnicky ?tít.
      
A new photoelectric photometer to determine intensities of the spectral lines of the solar corona is described.
      
The SPO is equipped with a 24-inch Cassegrainian telescope, a four-channel photoelectric photometer, a Wollaston prism, and a rotating half-wave plate.
      
The observations were carried out with a one-channel photoelectric photometer-polarimeter.
      
With a sensitive photoelectric photometer, observations of the sky twilight brightness have been carried out at different positions in the sky during high solar activity period.
      
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Cepheid variables CY Aqr and BE Mon were observed at the Purple Mountain Observatory with a photoelectric photometer during December 1959 and the first two months of 1960.The observations of CY Aqr (Table 1) made on four nights provide sufficient data for plotting five complete light curves (Fig.1) of this variable.The phase of these observations has been computed with Lange and Nekrasova's formula.We noticed that the maxima of the plotted curves do not fall on the zero phase,but show a shift of about...

Cepheid variables CY Aqr and BE Mon were observed at the Purple Mountain Observatory with a photoelectric photometer during December 1959 and the first two months of 1960.The observations of CY Aqr (Table 1) made on four nights provide sufficient data for plotting five complete light curves (Fig.1) of this variable.The phase of these observations has been computed with Lange and Nekrasova's formula.We noticed that the maxima of the plotted curves do not fall on the zero phase,but show a shift of about 0.05φin phase toward the left.In other words, the maximum light occurs four or five minutes ahead of the time predicted by this formula.

用紫金山天文台的60厘米反光望远镜和1P21光电倍增管所构成的光电光度计,我们在1959年底和1960年初,对 CY Aqr 及 BE Mon 进行了测光观测.得到 CY Aqr 的五条完整的光变曲线.我们采用了从1934年到现在的29个观测所得的极大历元来和公式计算的相比较.若不承认历元有跃迁的可能,那末任何线性公式,都难以满足这些观测数据的要求.我们按周期随时缩短的假设,得出下列比较满意的公式:Max⊙=I.D.2427658.4079十0~d.061038576E—(0~d.742×10~(-12))E~2.用前后将近两个月观测 BE Mon 所获得的数据,我们得到了这颗造父变星的光变曲线.变星总表引用所定0~d.421的周期是不正确的.根据我们观测所得到的周期是2~d.704.按这周期来整理于1935年所完成的目视观测,我们也得出了一个很象样的光变曲线.

Photometric observations of Nova Her 1963 were started in Peking on Feb.18, 1963,with a photoelectric photometer mounted on a 15 cm aluminized Cassegrain reflec- tor.The Nova was observed in the ultraviolet,blue,yellow,and red as well as through four relatively narrow-band filters whose commercial type designations being S43,S47, S50 and S53,with maximum transmissions of the cell-field lens-filter combination at about 4300,4550,4850 and 5230(?) respectively. Table 1 lists the types and parameters of the...

Photometric observations of Nova Her 1963 were started in Peking on Feb.18, 1963,with a photoelectric photometer mounted on a 15 cm aluminized Cassegrain reflec- tor.The Nova was observed in the ultraviolet,blue,yellow,and red as well as through four relatively narrow-band filters whose commercial type designations being S43,S47, S50 and S53,with maximum transmissions of the cell-field lens-filter combination at about 4300,4550,4850 and 5230(?) respectively. Table 1 lists the types and parameters of the filters.Figs.1 and 2 show the response curves of the cell (an unrefrigerated type EMI 6256 B tube) field lens combination when used with various filters as determined with a reflecting monochromator.The zero- point drift of our amplifier and the linearity of the amplifier-Dahua recorder combination are presented in fig.3. The star a=HR 6845 served as the principal comparison star,while μ Lyr and later c=HR 6853 was used as the check star.An attempt was made to reduce a part of our observations to the U,B,V-system using extinction and transformation equations in the form of equations (A),(B) and (C).u,b and y denote ultraviolet,blue and yellow magnitudes out of the atmosphere on our instrumental system,while u′,b′ and y′ denote the corresponding magnitudes inside the atmosphere.X is the air mass.The k's are extinction coefficients and the A's are transformation coefficients.Observations of selected U,B,V-standards were made on 10 nights in a manner after K.Serkowski. Narrow-band extinction observations were made on a single night by following γ Lyr through various zenith distances,from which a magnitude-air mass plot was obtained as shown in fig.5.The relation between the extinction coefficients so obtained and the maximum transmission wave lengths is shown in fig.6. As part of the discussion the probable errors of a single observation and that of the mean valuc of the natural magnitude differences in four colours (r=red) between c and a are listed in the third and fourth rows of Table 6,while a comparison of our U,B,V- data of a and c (second row from bottom) with those of other observers may be seen in Table 7. Tables 2—3 list the magnitude differences (Nova minus a) without differential ex- tinction correction,where ‘43’,‘47’,etc.denote observations through the filters S43,S47, etc.,and the values followed by colons represent uncertain results.The Nova entered the “transition” stage during the interval April 1—10,1963. A plot of magnitudes against log t (t being days after light maximum) as shown in figs.7—10 leads to values of t_c (t_c denotes the value of t at the points of intersection on these figures) increasing with effective wave lengths as indicated in table 4. For the star a we derived the values V=5.57,B-V=-0.15,and U-B=-0.42, each with p.e.=±0.01. Table 5 lists U,B,V-values of Nova Her 1963.The variations of V,B-V,and U—B are shown in figs.13—14.On the two-colour diagram (fig.15) our observations show the Nova moving in an extremely complicated manner,yet with a tendency first moving to the left downwards and,starting from early April,1963,moving to the right while down the diagram.It should be noted that large systematic differences exist be- tween our (B—V) values and those of the Italian observers,amounting to about 0(?)6,which could scarcely be explained by observational errors or by a strange behaviour of the Nova colour fluctuations keeping pace alternatively with the observations in Pe- king and at Asiago.Large differences of about the same order of magnitude seem also to exist between Babelsberg and Crimean(B-V) observations of Nova Her 1960. The situation seems to favour the point of view advanced by the Babelsberg observers that meaningful colour measurements of such abnormal stars as novae are impossible with ordinary wide-band photometry such as using the U,B,V-system. Adopting M_(V,max)≈3 and the date of maximum to be Jan.31,1963,one could make use of a relation to obtain an estimation of the visual absolute magnitude at maximum of Nova Her 1963 to be about -7.6,whereby we used the value t_(3.V)≈38 days according to our light-curve.In addition our observations show the Nova to be a fast one according to the classification listed by C.Payne-Gaposchkin.

北京天文台筹备处自制了一架光电光度计,在1963年2月到6月间进行了对1963年武仙座新星的光电观测.所用的波段,宽波段滤光片是 UG1、GG13、BG12、GG11和 RG1,窄波段是 S43、S47、S50和 S53.

By use of Kaare Aksnes’revised predictions,six events including two of mutual occultation and four of mutual eclipse have been observed photoelectrically.The equipment used consists of a photoelectric photometer mounted on a 60cm Cassegrain reflector and a GGll filter. Part 1.Mutual Occultation Various criteria and formulae for the occulted area S and the occulted bright- ness I_j corresponding to various occultation configurations illustrated in Fig A-F are given in(2)—(20). The brightness distribution...

By use of Kaare Aksnes’revised predictions,six events including two of mutual occultation and four of mutual eclipse have been observed photoelectrically.The equipment used consists of a photoelectric photometer mounted on a 60cm Cassegrain reflector and a GGll filter. Part 1.Mutual Occultation Various criteria and formulae for the occulted area S and the occulted bright- ness I_j corresponding to various occultation configurations illustrated in Fig A-F are given in(2)—(20). The brightness distribution over the apparent disk of the occulted satellite f(R) can be solved from the integral equations involving I_j. It is shown from Tab.4 and Tab.5 that the occulted satellite J2 has a basically uniform disk with some limb brightening.It could be interpreted that the occulted J2 has no atmosphere or has only such a thin atmospheric layer that no limb-dark- ening is caused.Its brightness distribution over the apparent disk is caused by its surface feature.One may imagine that a concave area exists near the center of the surface confronting the observers. The actual measure shows that the drop △V in visual magnitude for the two satellites combined is by far larger than the predicted value.(See Tab.2).The observations also show that Harris values of albedoes for Jovian satellites are ques- tionable. A comparison is made between the observed and the theoretical light curves(Tab. 6 and Tab.7). Part 2.Mutual Eclipse Link's photometric theory of eclipse is generalized. The simplifying method of computing i_N is described in Section 5.Three theore- tical light curves computed by this simplifying method and their comparison with observed light curves are shown in Fig.11—13. In the final part of this paper,the integral equations(90)and(91)of reduced curves are derived and the methods of solving these equations are discussed. The radius of J2 is computed by iterative process from equation(1)′—(5)′. The observational materials of 1973.8.9.102P are used in the computation.

对六次伽里略卫星相互掩食事件作了光电测光,使用仪器是60厘米返光望远镜和1P21光电倍增管,外加黄色滤光片GGll。本文分两个部分,第一部分讨论互掩,第二部分讨论互食。在第一部分中,给出了互掩的测光理论,提出了利用互掩光变曲线反求被掩木卫的亮度在圆面上分布的积分方程解法,讨论了被掩木卫(J2)的亮度在圆面上的分布、反照率、是否存在大气等问题,发现木卫2亮度的大幅度变化,计算了互掩的理论光变曲线。在第二部分中,推广了林克(F.Link)的关于行星和卫星的掩食测光理论。计算了互食的理论光变曲线。导出了关于归算曲线的积分方程。

 
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