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k-line
相关语句
  k线
     Research and Design of Automobile K-Line Communication Testing System
     汽车K线通信测试系统的研究
短句来源
     Development of Electronically-controlled Diagnosis Platform Based on K-Line
     基于K线的电控系统诊断平台开发
短句来源
     For the special testing requirements of K-Line products developed by automobile-electronic companies.
     针对汽车电子研发过程中对K线产品的特殊测试要求。
短句来源
     The main diagnosis type and judgement method of CRS(Common Rail System) were confirmed through the principle of expert system based on the study of common rail development, and the communication function between vehicle tester and practical CRS was realized by the way of K-line interface.
     在电控共轨系统开发的基础上,应用专家系统基本原理,对共轨系统故障诊断知识进行了合理分析,确定了共轨系统主要故障类型及判断方法,并在实际共轨系统上利用K线接口实现了与车辆诊断仪通讯功能。
短句来源
     K-Line is a industry bus standard which is widely used in automobile industry.
     K线是汽车工业当中广泛采用的一种通信总线标准,在许多场合都有着广泛的应用。
短句来源
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  k总线
     After that we have studied the K-Line communication protocol using in the self-diagnose system, windows network communication and database technology. We have made a hardware interface between K-Line and RS232 and carried out a method to realize a remote diagnosis system using the car ECU self-diagnose system.
     继而深入研究了汽车电子控制器自诊断K总线的通讯协议、Windows网络通讯以及数据库技术,制作了K总线到RS232的硬件接口,提出了一种将汽车电子控制器自诊断系统结合到远程诊断应用中去的方法。
短句来源
  “k-line”译为未确定词的双语例句
     AN ALGORITHM OF K-LINE LOCATION FOR BBL IN LSI/VLSI
     LSI/VLSI的任意元胞K行安置的算法
短句来源
     HOW TO READ THE K-LINE
     怎样识读K线图
短句来源
     On board diagnosis of ABS based on K-Line technology
     基于K-Line技术的汽车ABS在线检测
短句来源
     A K-line location algorithm for buillding block cells in LSI/VLSI is presented.
     本文提出一种适用于LSI/VLSI任意元胞布局的K行安置的算法。
短句来源
     For the purposes of acquiring the running parameters and trouble status of ABS, accelerating the procedure of development and debugging, implementing rapid diagnosis and test, on board diagnosis device is developed which fully satisfies the transmitting protocol of ISO-9141. Based on high-speed Flash microcontroller XC164CS from Infineon and K-Line technology, the device can be used in data stream communication, trouble code operation and component dynamic test.
     为了获取汽车防抱制动系统实时运行参数和故障状态,加速系统开发和调试过程,对系统实现快速诊断和测试,开发了其在线检测设备。 选用Infineon公司的闪存型高速微控制器XC164CS作为控制核心,数据传输基于K-Line技术,满足ISO-9141传输协议要求,可实现在线数据流通讯、故障代码操作、元件动态测试,并讨论了在线测试中的软件防干扰措施。
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  k-line
X-ray k-line absorption spectra of certain transition metals in their binary alloys with metalloids
      
The TON telescopes take K-line full-disk solar images of diameter 1000 pixels at a rate of one image per minute.
      
The data are from full-disk photometric images from CFDT1 (5 arc sec pixels) obtained at the Ca ii K-line λ = 393.4 nm.
      
In order to minimize the bias in finding faint facular features in continuum images, we have used coaligned images obtained in the Ca K-line to identify faculae.
      
The bright moss elements generally do not occur directly above the G-band or Ca?ii K-line bright points in the photosphere or lower chromosphere.
      
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Spectra of φ Per, ξ Tau, k Dra were obtained from December, 1978, to May, 1979. Several spectrophotometric and rotating comparison stars were both observed as well. All observations were made with the grating spectrograph attached to the 60/90 cm Schmidt telescope of the Beijing Observatory at Xing-Lung, giving a dispersion of 50 A/mm for Balmer visible region and 25 A/mm at Hα. The spectrograms were exposed on Kodak 103 aF and calibrated by the -28 prism spectrograph. The available plates are listed in Table...

Spectra of φ Per, ξ Tau, k Dra were obtained from December, 1978, to May, 1979. Several spectrophotometric and rotating comparison stars were both observed as well. All observations were made with the grating spectrograph attached to the 60/90 cm Schmidt telescope of the Beijing Observatory at Xing-Lung, giving a dispersion of 50 A/mm for Balmer visible region and 25 A/mm at Hα. The spectrograms were exposed on Kodak 103 aF and calibrated by the -28 prism spectrograph. The available plates are listed in Table 1. Using the 3CS microphotometer, all microphoto-metric tracings have been obtained.The profiles of Hα, Hβ, Hγ, Hδand Hε are shown in Fig. 1. The emission feature of Hα and Hβ in φ Per and ξ Tau are more intense than in K Dra. As for HeⅠ 4471, 4026, MgⅡ 4481 in spectrum of φ Per the vague and weak emissions are superposed over very wide and diffuse absorptions. In addition to evident NaⅠ D and CaⅡ K lines, the spectrum of ?Tau contains a number of lines of HeⅠ and SiⅡ.For four Balmer lines of the three Be stars, Table 2 gives three kinds of relative intensities which represent photosphere absorption, shell emission and shell absorption, respectively. The shell emission relative intensity of Hα, for instance, is eighteen times stronger than that of Hr in φ Per. Following Inglis-Teller formula or Unsold method which are used usually in analysis of stellar atmospheres, the electron concentration about these stars can be evaluated. The values lgNe and lgN2[H] are listed in Table 3. Here N, is the electron concentration and N2[H] is the number of hydrogen atoms on the second energy level above 1 cm2 of stellar surface by using the approximation of optically thin case.The variation of the ratio of the intensities of the blue and the red emission components, V/R, is a important parameter in Be stars. Figure 2 shows the variation of V/R. φ Per has the remarkable variation of V/R in Hα during our observed period. V/R > 1.25 was observed in January, 1979. But it swiftly decreased and was below 0.80 in February. Moreover, the double peak changed into single peak at the same time. Whereas in April the Hα of φ Per returned to double peak and the value of V/R increased rapidly. The V/R of Hα in ξ Tau still showed slowdown and V/R ~, 1 was retained in k Dra during the observed period. The V/R for other lines also were shown in Fig. 2.A study of line broadening interpreted as due to axial rotation of Be stars will yield only values of V sin i. The method used for obtaining the Vsin i is one suggested by Shajn and Struve. The absorption lines HeⅠ 4026 and MgⅡ 4481, were chosen for determination of Vsin i in φ Per, ξ Tau, k Dra and rotating comparison stars. More than two independent profiles were obtained for each of the stars considered. These were adjusted so that they have the same equivalent width as the appropriate standard profile and the comparisons were then made with the set of rotationally broadened profiles corresponding to the rotating comparison stars. Finally, the transformation into the Slettebak system can be made graphically with the use of commonly observed comparison stars. A set of rotationally broadened contours of HeⅠ 4026 for each Be star was built up (Fig. 3) and illustrated in Table 4. As compared with the work by Akira Uesugi and Ichiro Fukuda, the resultant values of Vsin i are conformable. The rotational velocity corresponding to a half-width of the emission Hα is the following:The progression about peak separation of emission lines in Balmer series, which were obtained in this paper, is congruent with the result given by Hutchings.The spectrum of ξ Tau in our observed period was compared with that of the B8Ia supergiant β Ori over the spectral range A 3500 to A 6600. The conclusion to be drawn from the spectrogram gevin by this paper is that at this time the state of excitation and ionisation in the shell of ξ, Tau was comparable to that in supergiant atmosphere of β Ori. The velocity of expansion in shell of ?Tau indicated by the NaⅠ D lines was 12 km/sec. In cons

自1978年12月至1979年5月间,我们用60/90厘米施米特卡氏反射光栅摄谱仪对φPer、ξTau、κDra进行了照相光谱观测。获得了电子浓度、自转速度、V/R变化等,并将ξTau同超巨星βOri进行了比较。 资料分析可得:在我们的观测期内,φPer存在着明显的气壳活动;ξTau处在相对宁静阶段,气壳缓慢膨胀;而κDra与“经典”的Be星相似。

Photoelectric observations of ξ Aur during the 1979-1980 eclipse were obtained at the Xing-Long Station of Beijing Observatory with the 60-cm reflector and its photometer from Nov. 17, 1979. The observations were made in six narrow-band and the standard UBV systems. The central wavelengths of the narrow-hand filters are in AA 3520, 3940, 4240, 5020, 6595 w and 6560 n A, respectively. The light curves were shown in fig. 1 and fig. 2. The second and third contact points were determined well from them. The moment...

Photoelectric observations of ξ Aur during the 1979-1980 eclipse were obtained at the Xing-Long Station of Beijing Observatory with the 60-cm reflector and its photometer from Nov. 17, 1979. The observations were made in six narrow-band and the standard UBV systems. The central wavelengths of the narrow-hand filters are in AA 3520, 3940, 4240, 5020, 6595 w and 6560 n A, respectively. The light curves were shown in fig. 1 and fig. 2. The second and third contact points were determined well from them. The moment of the mid-eclipse obtained turns out to be hel. J. D. 2444219. 643. The new formula for the moments of minima is Min.=J. D. 2444219. 643+972. 176 B. The photometric feature of the narrowband λ 3940 is consistent with that of spectroscopic observations of CaII K line. The photoelectric observations in λ 6595 w and 6560 n during totality indicate that it seems to be a pulsation, the period of which is several decades minutes. The values of our V, B-V and U-B for ξ Aur are in agreement with other observers'.

本文发表了ζAur在1979—1980年食期间进行的六个窄波段(峰值波长为3520,3940,4260,5020,6595(?)_ω和6560(?)_n)及UBV的光电测光结果。根据31个夜晚的有效观测资料得到了食的各不同位相的光变曲线。利用窄波段的光变曲线资料可以客观地确定食的第二、第三接触时刻,从而较准确地定出了食甚时刻,推算出ζAur食的新的历元公式 由图1可以明显地看出食的深度随观测的有效波长的减小而增加。窄波段3940的测光结果与分光观测的CaⅡ的K线变化一致,揭示了ζAur的K型超巨星在1979—1980年食期间色球活动比较激烈。 ζAur的UBV测光给出了关于ζAur系统的食深度及K型子星的V,B-V和U-B值,并与以前的结果作了比较,其结果相当一致。

We have developed a systematic method based on the statistical test theory and taking account of the '' ratio of signal-to-noise'' defined by Baheall"1 to deal with the problem of the identification of the redshift absorption line systems in the spectra of high redshift QSOs such as OQ 172. The key points of our procedures are summarized as follows:a) setting up the criteria for the identification (Ⅱ),b) dividing the whole redshift range into intervals, figuring out the configuration of the reference lines in...

We have developed a systematic method based on the statistical test theory and taking account of the '' ratio of signal-to-noise'' defined by Baheall"1 to deal with the problem of the identification of the redshift absorption line systems in the spectra of high redshift QSOs such as OQ 172. The key points of our procedures are summarized as follows:a) setting up the criteria for the identification (Ⅱ),b) dividing the whole redshift range into intervals, figuring out the configuration of the reference lines in each interval, computer searching the spectrum at step Az and counting the systems supported by k lines (Ⅲ),c) For each configuration calculating the theoretical probability (Ⅲ),d) For each configuration making the statistical test, finding out the systems which fall into the region of rejecting H0(Ⅳ),e) Filtering out the systems having high S value from the resulting systems in (d) (Ⅴ),f) Making the astrophysical analysis for the systems survived from the procedures above.The detail of (f) and other relevant problems will be discussed in a separate paper [10].

本文从统计检验理论和Bahcall的信噪比概念出发,提出了一种类星体吸收线红移系统的证认方法。其要点是:在一定的判据下计算谱线证认的理论随机概率;由此理论概率,按照统计检验的方法和信噪比的适当要求给出可供选择的红移系统;对这些可供选择的红移系统进行天体物理分析以最后确定出吸收线的红移系统。

 
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