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polarization filters
相关语句
  极化滤波器
     Theoretical Performance Analysis of Adaptive Polarization Filters
     自适应极化滤波器的理论性能分析
短句来源
     As for polarization filters, the important component of the polarization switchable Receive-Transmit(RT) system, the paper researches into the polarization filters from such aspects as polarization loss, filtering errors and amelioration of Signal Interference Ratio.
     对变极化收发系统的重要部件极化滤波器,本文从极化损失、滤波误差以及信干比改善等角度进行了详细地分析和研究。
短句来源
     By studying the transmission process of the estimation error in a polarization filter,a series of analytic formulae on the performances of adaptive polarization filters are derived,which stochastically reveal the relationship between the filtering performance and such factors as the signal-to-noise ratio clearly.
     通过研究极化估计误差在极化滤波器中的传播过程 ,导出了自适应极化滤波器理论性能的解析公式 ,清楚地揭示了滤波性能与信噪比等因素的统计关系 .
短句来源
  “polarization filters”译为未确定词的双语例句
     Circular Polarization Filters Made of Cholesteric Liquid Crystal Thin Films
     胆甾相液晶薄膜圆偏振滤光器
短句来源
  相似匹配句对
     polarization.
     偏振条件下为非拉曼活性。
短句来源
     Compensation of Polarization Mode Dispersion by the Filters
     滤波器对偏振模色散的补偿
短句来源
     Research of Double-Pass Polarization Interference Filters
     双通偏振干涉滤光片的研究
短句来源
     Wavelet filters
     小波滤波器组
短句来源
     Selection of Filters
     过滤器的选择
短句来源
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  polarization filters
A technique has also been developed for determining the position of the plane of polarization by means of isophotes obtained with polarization filters.
      
The 0R0 geometry of the optical arrangement and the use of crossed polarization filters for blocking specular reflectance makes it possible to use the Kubelka-Munk function for quantifying the optical measurements.
      
Sections were examined under a light microscope using polarization filters.
      
Polarization filters are used in front of the projectors and the eyes to apply the separation.
      
Polarization filters are used to reduce reflected skylight in the instrument's field-of-view.
      
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When P waves from distant earthquakes meet a velocity discontinuity in the earth's crust and upper mantle, they give rise to a series of converted PS waves besides PP refracted waves. The difference of arrival times between such PS and PP waves can be used to determine the structures in the earth's crust and upper mantle.For the first time, method converted waves from distant earthquakes have been tried in the Shiahjin-Gautarng (夏津-高唐) region of western Shandung, Province and in the Changpirng (昌平) area west...

When P waves from distant earthquakes meet a velocity discontinuity in the earth's crust and upper mantle, they give rise to a series of converted PS waves besides PP refracted waves. The difference of arrival times between such PS and PP waves can be used to determine the structures in the earth's crust and upper mantle.For the first time, method converted waves from distant earthquakes have been tried in the Shiahjin-Gautarng (夏津-高唐) region of western Shandung, Province and in the Changpirng (昌平) area west of Peking.Polarization filtering was employed to analyze the seismic data in order to increase the reliability in identifying the PS phases. As a result, the crustal structures in these two regions have been found and it is indicated that the main deep discontinuities thus obtained are essentially the same as those determined by deep seismic sounding experiments using explosions.

当远震P波通过地壳、上地幔速度界面时,除了产生PP型折射波,还产生一系列PS型折射转换波.这类PS转换波与初至P波之间的到时差,可用来测定地壳和上地幔构造. 转换波测深法首次在我国鲁西夏津—高唐地区和京西昌平地区进行了试验应用.为提高转换波震相识别的可靠性,在资料分析中采用了偏振滤波的方法.工作结果获得了上述两地区的深部构造剖面图.转换波法与爆炸地震法所得结果之对比表明,两者的主要界面基本一致.

Theory and experiments of a new stereoprojection technique that uses a white-light optical image processing system are described. The stereoprojection can be accomplished in two steps: (1) Spatial encoding of stereoscopically-coupled images, and (2) spatial polarization filtering at the Fourier plane in a white-light optical image processor. Comparing with existing stereoprojection methods, the present technique requires only one projector and a single piece of encoded film, therefore it is much simpler...

Theory and experiments of a new stereoprojection technique that uses a white-light optical image processing system are described. The stereoprojection can be accomplished in two steps: (1) Spatial encoding of stereoscopically-coupled images, and (2) spatial polarization filtering at the Fourier plane in a white-light optical image processor. Comparing with existing stereoprojection methods, the present technique requires only one projector and a single piece of encoded film, therefore it is much simpler and more economical for practical applications.

本文提供了一个用白光图像处理系统作立体投影的新方法,它包括将两张立体透明图像编码在一张感光片上和在白光图像处理系统的傅里叶频谱平面上采用偏振滤波的新技术。与一般传统的立体投影技术相比较,它可节省拷贝片一倍,并且只用一个投影光学系统。

Among the various types of solar magnetographs the video-magnetograph has the highest temporal resolution. This instrument uses an interference-polarization filter, whose pass-band is situated in the wing of a magneto-sensitive spectral line. Due to the technical difficulties in making narrow pass-band filters the working line of video-inagne-tographs has been chosen to be PeI λ5324.191. This is because its total half-width is about 0.3 A, much larger than those of other magneto-sensitive lines....

Among the various types of solar magnetographs the video-magnetograph has the highest temporal resolution. This instrument uses an interference-polarization filter, whose pass-band is situated in the wing of a magneto-sensitive spectral line. Due to the technical difficulties in making narrow pass-band filters the working line of video-inagne-tographs has been chosen to be PeI λ5324.191. This is because its total half-width is about 0.3 A, much larger than those of other magneto-sensitive lines. In order to justify its suitability to the observations of magnetic fields, an investigation of the properties of this line is performed in this paper.For a long time in the past the working line adopted in solar magnetic field measurements was FeI λ5250.216. However, by the end of the sixties, it was noted by astronomers that this line is very sensitive to temperature. Therefore its variations in magnetic regions are caused not only by magnetic fields, but also by the change of temperature. So it is difficult to deduce information of magnetic fields with observations made in this line. For this reason, λ5250 has been discarded in solar magnetic field measurements. In order to clarify whether this is also the case for λ5324, we should calculate the temperature sensitivity of this line. Yet it has to be pointed out that computations of the profile and its sensitivity to temperature are especially difficult for λ5324. This is because its profile is very deep in the center-its residual intensity at line center is only 0.17. This means that the absorption in the central region is unusually strong. Hence the variations of parameters of this line from center to wings are very large and then the step length of the numerical integration of the equations of transfer should be taken to be sufficiently small. This leads to a great increase of computer time. Maybe due to this reason up to the present the line λ5324 has not been studied carefully.In the second section of this paper we have got forλ5324 a numerical solution of Unno's equations of transfer of the Stokes parameters for sunspots. This provides us the profiles of the parameters I, Q and V and serves as the basis of our study.In section 3, the quantity of magnetic intensification ΔWλof λ5324 has been calculated. ΔWλ is defined to be equal to Wλ(H) - Wλ(0), where Wλ(0) is the equivalent width in the absence of magnetic fields, i.e. H=0. It has been found that ΔWλ depends on both H and γ. This can be seen in Fig. 4.In section 4, we have computed the temperature sensitivity of λ5324. This quantity is denoted by Wu/ Wph, where Wu and Wph are the equivalent widths of one and the same line in a sunspot umbra and in the photosphere. Adopting Kneer 's sunspot model, we have found that the temperature sensitivity of λ5324 is moderate in comparison with some other magneto-sensitive lines (see Table 1). Concretely speaking, Wu/Wph = 1.97 for λ5324. But this value depends on the model of the atmosphere. For Zwaan's model of sunspot umbra, we have got for the same line Wu/Wph=2.13.In conclusion we may say that the profiles of the Stokes parameters of the magneto-sensitive line Fel λ5324.191 are sensitive to magnetic fields. Its I-profile exhibits evident Zeeman splitting in the magnetic fields of sunspots. Its magnetic intensification is large enough and it is not very sensitive to temperature. Taking all these characteristics into consideration, we may conclude that it is rather adequate to use Fel λ5324.191 as the working line of video-magnetographs.

为了判断视频磁象仪的工作谱线 FeIλ5324.191 对磁场观测的适用性,本文由海野方程组的数值解,计算这条谱线的斯托克斯参数轮廓,并推算它的磁场增强量和温度敏感度。

 
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