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radio
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  射电
    Radio Observational Studies of High Luminosity AGNs and the Dim Galactic Center Object Sgr A~*
    高光度活动星系核和暗弱银心天体Sgr A~*的射电观测研究
短句来源
    OBSERVATIONS OF SOLAR RADIO EMISSION AT 146 MHZ INSTRUMENTAL AND DATA ANALYSIS
    146兆赫太阳射电观测——仪器和数据分析部分
短句来源
    RADIO OBSERVATION OF THE SOLAR ECLIPSE OF SEPTEMBER 22,1968 AT THE WAVELENGTH OF 21 CM
    1968年9月22日日食21厘米射电观测
短句来源
    A STATISTICAL ANALYSIS FOR QUASARS WITH RADIO COMPONENTS STRUCTURE——Ⅰ.Redshift-Magnitude Relation
    有射电子源结构类星体的统计分析 Ⅰ.视星等红移关系
短句来源
    A STATISTICAL ANALYSIS FOR QUASARS WITH RADIO COMPONENTS STRUCTURE Ⅱ.RELATIONS OF ABSOLUTE VISUAL MAGNITUDE,ABSOLUTE RADIO MAGNITUDE AND COLOUR INDEX DIFFERENCE Q WITH THE LINEAR DISTANCE BETWEEN COMPONENTS,AND THE ASSOCIATED EVOLUTION FEATURE
    有射电子源结构类星体的统计分析 Ⅱ.绝对视星等、绝对射电星等和色指数差Q与子源线距的关系以及有关的演化特征
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  “radio”译为未确定词的双语例句
    Research on the Radio Heliograph Array Design
    日像仪天线阵系统设计研究
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    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
短句来源
    RADIO OBSERVATION AT THE WAVELENGTH OF 3 CM DURING THE SOLAR ECLIPSE OF SEPTEMBER 22,1968.
    1968年9月22日日食3厘米波段强度观测
短句来源
    THE NONLINEAR SCATTERING MECHANISM OF THE SPECTRUM OF THE TYPE Ⅳ SOLAR DECIMETRIC RADIO BURSTS
    太阳Ⅳ型分米波爆的非线性散射机制
短句来源
    THE RELATION BETWEEN SOLAR PROTON EVENTS AND SOLAR RADIO METRIC WAVE I-TYPE SOURCES
    太阳米波Ⅰ型源与太阳质子事件的关系
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  radio
Efficiently implemented in field programmable gate arrays (FPGA), the generator prototype of the proposed sequence has been realized and incorporated into fast FH radio.
      
In this method, 2-D feature information was constituted by using radio frequency and time-of-arrival, which analyzed the feature of radar pulse sequences for the very first time by employing structure function and empirical mode decomposition.
      
The experiment shows that the method can efficiently extract the frequency of a period-change radio frequency signal in a complex pulses environment and reveals a new feature for the signal sorting of interleaved radar pulse serial.
      
The Doppler spectral broadening resulted from non-stationary movement of target and radio-frequency interference will decrease the veracity of target detection by high frequency ground wave (HFGW) radar.
      
The results indicate that the preprocessing not only makes the system acquire a higher ability of target detection but also suppresses the radio frequency interference by 6-7 dB.
      
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After summarizing the sources and effects of time lag in radio transmissions and receptions, we suggest a simple but accurate method to determine this particular type of error as occured in a radio receiver (Fig. 4 Section 3). The results proved to be satisfactory and were discussed in full.

本文中讨论了收時系统遲滯差的來源及其影響。并在適应一般的設備條件下,提出一精簡單而比较精确的测定方法。對於这種方法的試驗結果,我們作了详尽的比较与讨论。

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...

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。

From a large number of H_a photographs of limb flares,fifteen have been selected for reduction.The films were obtained with the standard Lyot-type Chromospheric patrol telescope at the Purple Mountain Observatory during the years 1959—1960. The photometric and positional measurements of limb flares have led to the following conclusions: (1)There are violent radial ejections of matter during the flash-phase of the flare. Usually a part of the flare is ejected to distances ranging from 2×10~4 km to 2.5×10~5 km...

From a large number of H_a photographs of limb flares,fifteen have been selected for reduction.The films were obtained with the standard Lyot-type Chromospheric patrol telescope at the Purple Mountain Observatory during the years 1959—1960. The photometric and positional measurements of limb flares have led to the following conclusions: (1)There are violent radial ejections of matter during the flash-phase of the flare. Usually a part of the flare is ejected to distances ranging from 2×10~4 km to 2.5×10~5 km above the base of the chromosphere. (2)The mean velocity of ejection is of the order of 30 km/sec—400 km/sec.The maximum velocity appears in the initial stage of ejection and decreases later on.The acceleration of ejection is supergravitational. (3)The ejective motions of flares are regular and apparently connected with the magnetic fields of the active regions. (4)During the flash-phase of the flare the velocity of ejection varies directly with the rate of increase of brightness. In conclusion,it is noted that the appearance of radio events is closely related to the ejection.

在大量的 H_α边缘耀斑电影胶卷中,为了精炼起见我们选取了15套.电影胶卷是在1959年—1960年期间用紫金山天文台的利奥型色球望远镜拍摄的.边缘耀斑的光度和定位测量得出下列结果:(1)在耀斑的闪光阶段存在着剧烈的径向物质抛射,常常耀斑的一部分被抛射到色球层之上高达2·10~4公里到2.5·10~5公里处.(2)抛射的平均速度是30公里/秒—400公里/秒的数量级,最大的速度出现在抛射的初始阶段,抛射的加速度是超引力的.(3)耀斑的抛射运动是有规则的,且明显地与活动区的磁场有关.(4)在耀斑闪光阶段,抛射速度直接地随亮度增加的速率而变化.最后,注意到了射电事件的出现与抛射密切有关.

 
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