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temporal resolution
相关语句
  时间分辨率
     Temporal resolution is 1ms and spatial resolution is about 5mm.
     时间分辨率可达1ms,空间分辨率约为5mm。
短句来源
     The highest temporal resolution of the apparatus was 0.1 μs.
     仪器的最高的时间分辨率为0.1μs。
短句来源
     By using the ultrafast electro-optic sampling system with temporal resolution as high as 16.7 ps and voltage sensitivity of 0.26 mVHz~(-1/2), in which a semiconductor laser of 1.3 μm wavelength is used as a source of sampling, the microwave signals of 1~5 GHz and the dispersive characteristics of the coaxial cable have been measured.
     利用半导体激光器作为采样光源的超高速电光采样测试系统(时间分辨率最高可达16.7ps,电压灵敏度为0.26mVHz~(-1/2)). 测量了1~5GHz的微波信号和同轴电缆传输线的色散展宽.
短句来源
     A HCN laser is used as the light source with 3.4m cavity length,100mW output power and 100μs temporal resolution.
     干涉仪的光源是一台腔长3.4m、连续辉光放电的HCN激光器,波长337μm,输出功率100mW,测量的时间分辨率为100μs。
短句来源
     Diagnostic accuracy of noninvasive coronary imaging using 16-detector slice spiral computed tomography with 188 ms temporal resolution
     时间分辨率为188ms的16多层探测器螺旋CT非侵入性冠状动脉成像的诊断精确性研究
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  时间分辨
     High Temporal Resolution H_α and Off-band Observation on 2B / X1.3 Flare of AR 5047 on June 24,1988
     1988年6月24日AR5047活动区中2B/X1.3耀斑的高时间分辨H_α和偏带观测结果(英文)
短句来源
     Information on Te (r,t) can be obtained through a horizontal viewing system with the spatial resolution of 0.5cm and temporal resolution of 50μs.
     该系统具有研究等离子体温度参数的时空演化能力,空间分辨可达0.5cm,时间分辨达50μs。
短句来源
     This paper presents the time resolved spectrum with high temporal resolution (~10ps) and spectral resolution (~ 0.6 A) of 2ω_0 harmonic emission at 90°to the laser axis.
     本文报道沿与光轴成90°方向拍摄的2ω_0谐波时间分辨光谱。
短句来源
     Experimental results show that the diagnostics are easy to bring into effect,with temporal resolution of 50 ps,spatial resolution of 10~20 μm and energy resolution power of a few tens.
     实验过程和结果表明,该方法系统结构和实施都较为简单,可以比较容易地在分幅相机微带上获得经平面镜反射的靶目标针孔像,实现~50ps的时间分辨、10~20μm的空间分辨及几十倍的能量分辨.
短句来源
     05nm , respectively. The temporal resolution is ~30ps. Finally, the evaluation is given.
     用国产软X光扫描相机作时间分辨记录时,谱分辨为0.05nm,时间分辨本领约为30ps。
短句来源
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  时间分辨力
     Temporal resolution of the system is 6.5 ps, nonlinearity is 2.60%, and the measurable time range is from ten picoseconds to tens of nanoseconds.
     该系统的时间分辨力达到6.5ps,非线性为2.60%,可测量的时间范围从十几皮秒到几十纳秒。
短句来源
     The close focusing electro-optical system and avalanche diode circuit used in the system makes the camera attain the following specifications: energy spectrum response range of UV -1keV, spatial resolution of static state 15Lp/mm and dynamic state 5Lp/mm, temporal resolution of 500ps.
     系统设计中采用近贴聚焦电子光学系统和雪崩管电路使得目前所能达到的指标为:能谱响应范围紫外~1keV,空间分辨力静态15Lp/mm,动态5Lp/mm,时间分辨力为500ps。
短句来源
     The improved SPT techniques not only can accurately measure the light intensity of the receptor,but also provide a high temporal resolution.
     经改善的 SPT技术不但可以精确测量受体的光强 ,而且还可以提供高时间分辨力
短句来源
     Results:The change of the quality of CT perfusion images and the value of CBV could be omitted when the temporal resolutions were decreased within a certain extent (≤2s),but the values of CBF and MTT changed remarkably following the decrease of the temporal resolution.
     结果:降低时间分辨力在一定范围内(≤2s)对各灌注 参数图的图像质量以及CBV绝对值的测量影响不大,但对参数CBF和MTT的绝对值测量产生显著影响。
短句来源
     The Quality of CT Perfusion Image of Low Temporal Resolution
     降低时间分辨力对CT灌注图像的影响
短句来源
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  “temporal resolution”译为未确定词的双语例句
     Image quality and diagnostic accuracy of non-invasive coronary imaging with 16 detector slice spiral computed tomography with 188 ms temporal resolution
     利用帧分辨率为188ms的16排螺旋CT进行无创冠状动脉显像的图像质量和诊断准确性
短句来源
     microwave type-Ⅲ bursts have been observed by using the solar radio synchronous observational system with high temporal resolution at 1.42GHz, 2.13GHz, 2.84GHz and 4.26GHz in Yunnan Observatory during January 1990 to January 1994. The characteristics (such as durations, frequency drift, associated phenomena) of them are introduced briefly.
     云南天文台“四波段(1.42GHz,2.13GHz,2.84GHz和4.26GHz)太阳射电高时间同步观测系统”在1990.1~1994.1期间,观测到5个具有短时标漂移结构的射电爆发事件,也就是微波Ⅲ型爆发。
短句来源
     The temporal resolution was 2 hours and 30 minutes.
     采样频率分别取为 30分钟和 2小时。
短句来源
     The temporal resolution of the system is about 2. 5 fs and the sensibility is in the scale of microvoltages.
     仪器的分辨率达2.5fs,测量灵敏度达微伏量级.
短句来源
     Numerical simulation is made for extremely heavy rain and meso-β scale low vortex in Huangshi of Hubei province during 21-22 July 1998 using a meso scale rainstorm model MRM1. High spatial and temporal resolution model-output physical fields are analyzed according to the conservation principle of moist potential vorticity.
     利用中尺度暴雨模式MRM1,对1998年7月21、22日湖北黄石的β中尺度低涡及特大暴雨进行数值模拟,采用湿位涡守恒原理对模式输出的高时空分辨率物理量场进行分析。
短句来源
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  temporal resolution
The results obtained agree with the data of ionospheric parameter measurements conducted earlier by methods with high temporal resolution.
      
The upper limit of the gauge's operating range is 6 × 1017cm-3at a spatial resolution in the jet cross section of 0.5 mm and a temporal resolution of ≤15 μs.
      
These detectors will be used as neutron-flux monitors in a multichannel neutron collimator for obtaining the spatial characteristics of a plasma source of thermonuclear neutrons with a 1-ms temporal resolution.
      
A double-pass dispersion interferometer based on a 9.6-μm CO2 laser with a sensitivity of ? nel?min ~ 1 × 1013 cm-2 and a temporal resolution of ~50 μ s, designed to measure linear plasma density, is described.
      
The range of density measurements is 0.7 × 1012-0.7 × 1014 cm-3, the measurement accuracy is no worse than 1%, and the temporal resolution reaches 30 ns.
      
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Under the assumption of the propagation of Alfven waves we have in this paper numerically solved the system of equations of transfer of Stokes parameters I, Q and V and calculated the effects of Alfven waves on the magneto-sensitive line FeI λ6302. 499 in the spectra of sunspots. According to the theory of the cooling of sunspots recently proposed by E. N. Parker et al., the missing energy flux in spots is transported outwards mainly by Alfven waves. The results of our calculations show that if this is true,...

Under the assumption of the propagation of Alfven waves we have in this paper numerically solved the system of equations of transfer of Stokes parameters I, Q and V and calculated the effects of Alfven waves on the magneto-sensitive line FeI λ6302. 499 in the spectra of sunspots. According to the theory of the cooling of sunspots recently proposed by E. N. Parker et al., the missing energy flux in spots is transported outwards mainly by Alfven waves. The results of our calculations show that if this is true, Alfven motions should become the most important mechanism of the broadening of spectral lines and give rise to remarkable oscillations of the profiles of all the Stokes parameters within the period of Alfven waves, as shown by Figs. 2—5. Besides the profiles of Stokes parameters at various phases in oscillations, we have also calculated the mean profiles averaged over the whole period of Alfven wave motions. Owing to the limited spatial and temporal resolution of observations it is rather difficult to discern such oscillations directly. Therefore we have designed some other methods of observational verification. They are described in section 4. Besides this, we have in section 5 proposed a method of estimating the energy flux of Alfven waves be means of the observed profiles of the magneto-sensitive lines in the spectra of sunspots. Our calculations have been carried out on the assumption that the plasma of sunspots permeated by Alfven waves is incompressible. This is, of course, an approximation. Nevertheless, we have in section 3 shown that the errors caused by this assumption are small and tolerable. Under the influence of Alfven waves the Zeeman splitting of magneto-sensitive lines should also vary periodically. But, as we have pointed out in section 4, this effect is, small and may be detected only with very accurate apparatus.

本文在阿尔文波传播的假设条件下,求解斯托克斯参数转移方程组,计算阿尔文波对太阳黑子光谱中磁敏线Felλ6302.499的作用,并提出用观测资料对理论计算结果进行检验,以及估计阿尔文波流量的方法。

Three sequences of active regions pictures with high spatial and temporal resolutions,obtained from monitoring continually active regions in white-light during flare process in a period of half a year,show that the energy necessary for flare is rapidly bnought from beneath the photosphere.Phenomena revealed by these pictures include the rapidly changing magnetic field ejected from umbrae and the enhancement of whlte-light emission within sunspot group.The energy provided by them is sufficient to supply...

Three sequences of active regions pictures with high spatial and temporal resolutions,obtained from monitoring continually active regions in white-light during flare process in a period of half a year,show that the energy necessary for flare is rapidly bnought from beneath the photosphere.Phenomena revealed by these pictures include the rapidly changing magnetic field ejected from umbrae and the enhancement of whlte-light emission within sunspot group.The energy provided by them is sufficient to supply a large flare with 10~(32) ergs.We believe that complex flare phenomena are caused by complex photospheric disturbences. The energy flow brought from sub-photosphere has some horizontal effects on those sunspots which were located on its passage,they being subject to deformatin,disintegrating and even completely disappearing within several minutes to hours.

根据半年多用高时间分辨率和高空间分辨率的光球观测监视太阳活动区的结果,我们以三组和耀斑有关的光球变化照片来表明耀斑过程中有能量从光球下层快速出来,表现形式为从黑子本影“抛出”磁场和黑子群内白光辐射增强,它们足以供给10~(31)—10~(32)尔格大耀斑的能量。耀斑前后及耀斑过程活动区光球变化在空间、时间和现象本身的多样性是造成复杂的耀斑现象的根本原因。从光球下层快速出来的能流在水平方向有明显的动力学效应,它使在其通道上的小黑子变形、瓦解、甚至在几分钟至几小时内消失。

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...

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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