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astronomical
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  天文
    THE APPLICATION OF A LASER SPHERICAL WAVE INTERFEROMETER IN ASTRONOMICAL OPTICS
    激光球波面干涉仪在天文光学中的应用
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    Influence of M_2 Tide of Near Sea in China on the Astronomical Time and Latitude Determination
    我国近海M_2潮波对天文时纬观测的影响(摘要)
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    New System of Astronomical Constants
    新天文常数系统
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    The Infrared Detectors for Astronomical Purpose
    天文用红外探测器
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    A Far Infrared Photometer for Ground Based Astronomical Observations
    一个地面天文观测的远红外光度计
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  “astronomical”译为未确定词的双语例句
    1978 MEETING OF THE CHINESE ASTRONOMICAL SOCIETY
    中国天文学会1978年年会简况
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    The Catalogue Obtained with the Photoelectric Astrolabe (Type Ⅰ) in Shaanxi Astronomical Observatory
    陕台光电等高仪(Ⅰ型)初始星表(摘要)
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    Chinese Astronomical Society Symposium No, 1: 《The Application of statistical Methods to Satellite Dynamics》 (Kunming, April 1983)
    中国天文学会学术会议(序号1):《统计方法在卫星动力学中的应用》讨论会(1983年4月,昆明)
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    Chinese Astronomical Society Symposium No.3: 《Astronomical Popularizat-ion Meeting》 (Beijing, May 1983)
    中国天文学会学术会议(序号3):普及工作会议及学术报告会(1983年5月,北京)
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    Chinese Astronomical Society Symposium No.5: 《Radioastronomy》 (Beijing, September 1983)
    中国天文学会学术会议(序号5):射电天文学术讨论会(1983年9月,北京)
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  astronomical
The work is based on wide-angle polarimetric CCD-observations of the twilight sky near zenith in the U, B, V, and R bands, which were carried out in summer 2000 at the South Laboratory of the Moscow Shternberg Astronomical Institute.
      
A brief review of publications on the problem of two fixed centers is given, including its generalizations and astronomical applications.
      
The measurements were carried out in 2002 and 2003 at the Southern Laboratory (Crimea) of the Sternberg Astronomical Institute.
      
A Prototype of a Neutron and γ-Ray Spectrometer for Studying Solar Activity at Distances of 0.5 Astronomical Units to 25 Solar R
      
A laser interferometer-deformograph with a 75-m-long arm has been developed by Moscow State University's Sternberg State Astronomical Institute to record and study lithospheric deformations over a wide frequency range.
      
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As in general in all time service works, the problem is to obtain and keep an accurate time, to determine the corrections of standard clock and to transmit time signals. This present report is concerned only with the last two items. At Zi-Ka-Wei Observatory, radio method was introduced into time service in 1914. Some rigorous changes occured in 1926, a number of instruments were installed. Many of them are still in use. In 1940, the observatory began to transmit rhythmic signals twice a day. From then on until...

As in general in all time service works, the problem is to obtain and keep an accurate time, to determine the corrections of standard clock and to transmit time signals. This present report is concerned only with the last two items. At Zi-Ka-Wei Observatory, radio method was introduced into time service in 1914. Some rigorous changes occured in 1926, a number of instruments were installed. Many of them are still in use. In 1940, the observatory began to transmit rhythmic signals twice a day. From then on until December 1950, no further developments were made. The main instruments we had in 1950 were: a 80mm Prin transit with impersonal micrometer, two Leroy pendulums as standard clocks, three astronomical clocks and their slaves, equipments for receiving and recording time signals, etc. Since 1952, we began to make some improvements, especially on rhythmic signals. First, we converted a common clock into a "transmitting clock" to obtain 61 impulses in every minute and second by making use of photoelectric arrangement (Fig. 1), we succeeded to raise the accuracy of our signals. To improve signal accuracy further, we have to deal with various sources of errors which are conditioned by our equipments. The most important among these are: 1. error in prediction of corrections of the standard clocks, 2. error in the adjustment of the transmitting clock and 3. time lag in transmission. In consequence of last three-year's research, these errors are reasonably reduced. The first two are now±0~s.007 and ±0~s.005 respectively and the last is small. Accordingly, the deviation of time signals XSG has been supposed to be±0~s.01. However, this is not enough for the requirement. The more efforts are being made to bring further improvements. But as the requirements for signal accuracy is far above what the present installation can offer, some new equipments are ordered and they will joint in force with the old ones in the nearest future. Since February 1954, Zi-Ka-Wei Observatory has cooperated with the time service departments in Soviet Union. This has been helpful to our works in every way.

授時包括测時、守時和播時三个主要方面。在時號的发播中包含了预報主钟改正量的差误,工作钟的調節誤差和電路遲滯变化等三种誤差。如果使用石英钟及有關设备,这就可基本解决。各台站在其天文观测基础上订定的時號改正數也包含有偶然差和系统差,比較全面解決的只有蘇聯和国際時間局这两个标准系统。徐家匯觀象台授時工作歷史很久,作了一些工作,但抗戰以來,郎停滯不前,直到人民政府接办,才逐步在原有基礎上開展了改進。幾年来主要是改裝了一具工作钟,裝置光電设备以发播科学式時號,對時号精确度解决了秒距誤差和五分间誤差。工作钟的调节誤差被其本身品質所限,仍未解决,只是在加強值班工作之后,有了一定限度的提高,目前約為±0~s.005,在预报主钟改正量時,也有很大程度的不稳定,約為±0~s.007。所以時号的精确度在±0~s.01左右。要进一步提高质量,满足要求,有待於新設備的增添使用。在時号改正數方面,所存在的相當大的系统差,可採用蘇聯或国際時間局系統的改正數來避免。

The optical system with two aspherical mirrors essentially for astronomical use is discussed by the third-order aberration theory. Conditions for correcting aberrations with any combination are derived. All two-mirror systems which had been suggested in the past are included.

本文用三级象差理论讨论了由两个二次曲面反射镜组成的,主要是天文望远镜的光学系统。导出了各种联合消象差的条件。概括了以往所有提出过的两镜系统。

This paper describes the optical principles,methods of usage,precautions and applications in testing of astronomical optical surfaces by means of,an interferometer, the source of which is a He-Ne gas laser tube.Some merits of this method are therein pointed out. At present,this apparatus is used mainly for the examination of the perfectness of convergent spherical wave surface with aperture angle≤1:3,hence it can be used for the non-contact direct test of aluminized or unaluminized concave mirrors with...

This paper describes the optical principles,methods of usage,precautions and applications in testing of astronomical optical surfaces by means of,an interferometer, the source of which is a He-Ne gas laser tube.Some merits of this method are therein pointed out. At present,this apparatus is used mainly for the examination of the perfectness of convergent spherical wave surface with aperture angle≤1:3,hence it can be used for the non-contact direct test of aluminized or unaluminized concave mirrors with any aperture.In combination with supplementary mirrors one can test flat mirror,various aspherical mirrors used in astronomical telescopes,homogeneity of medium(e.g.op- tical glass),quality of optical systems,state of optical axis alignment and assembly deformations.With this interferometer one can also determine the wave surface dif- ferences of an objective with the laser wavelength presently used(6328.(?))and mea- sure some aberrations.

本文叙述了用氦氖气体激光管做为光源的干涉仪光路原理、使用方法、注意事项及在天文光学镜面制造中的应用.该仪器现在专用来检验张角≤1:3的会聚球波面的完善性.因此可以用来无接触的直接检验任意口径的镀铝或未镀铝的凹球面镜;加入辅助镜后可以检验平面镜、天文望远镜用的各种非球面镜、介质(如光学玻璃)的均匀性、光学系统的质量、光轴校正及安装变形情况;也可给出物镜对于现用激光波长(6328)的波面差及测出某些象差.

 
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