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  “lines structure”译为未确定词的双语例句
     By using demand & supply theory to analysis the imbalance problem of our countrys civil aviation transportation market, I pointed out that our current city-pair network can no longer satisfied the market requirement, the key to solve the problem lay in the adjustment of air lines structure.
     本文运用需求、供给分析理论,对我国民航运输市场的失衡进行分析,指出我国目前的城市对航线网络结构已不适应当前民航运输市场的需要,解决问题的关键在于航线结构的调整。
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     In the fierce competition, Aotai Electric re-arranges quickly the lines structure to increase quality, promoting manufacturing technology and optimizing performance of welding machines as well as enlarging enterprise size and enhancing competitiveness.
     在激烈的市场竞争中,奥太公司加快了产品结构调整,使焊机质量、性能、制造技术水平大大提高,企业规模不断扩大,竞争能力不断增强,并适时抓住机遇加紧制定海外市场营销战略,积极参与国际竞争。
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     The airfield is recognized according to the parallel lines structure features of main and additional runways and structure feature of Chinese “ri(sun)”, “mu(eye)” words consisting of the runways and the paths connecting with them.
     然后根据机场主、辅跑道的平行直线特征 ,与它们之间相连的道路一起构成“日”字、“目”字等结构特征 ,识别出军用机场 ;
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     " ,the structure
     兼及了“V他+……”结构的特征。
     On ITS Structure
     论ITS的结构体系
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     And analyzed the structure characteristic of the two lines.
     分析了2种生产线配套辅机的结构特点。
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     The Beauty of Lines and Harmonious and Balanced Structure in Chinese Characters
     汉字的线条美和结构和谐均衡美
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     Industry Lines
     硅谷、深圳高新技术产业带文化与环境建设断想
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Magnetic field topology and field lines structure in the Dynamic Ergodic Divertor of TEXTOR-94
      


The structure of cometary dust tails is studied in the frame of mechanical theory with special regards to threedimensional treatment of the problem. We begin with the reexamination of orbit mechanics of cometary particles to derive a set of formulae convenient to subsequent discussions and calculations.Mak- ing use of Hamilton's integral b,we have obtained,for example,the equation of orbit in a vectorial form with generalization respecting to force parameter μ(Part 2).On the basis of Part 2,we consider...

The structure of cometary dust tails is studied in the frame of mechanical theory with special regards to threedimensional treatment of the problem. We begin with the reexamination of orbit mechanics of cometary particles to derive a set of formulae convenient to subsequent discussions and calculations.Mak- ing use of Hamilton's integral b,we have obtained,for example,the equation of orbit in a vectorial form with generalization respecting to force parameter μ(Part 2).On the basis of Part 2,we consider such problems as follows:the relation between initial conditions together with μ and the orbit characteristics;the algorithm for computer-calculation of the motion of particles some interesting features of ele- mentary space distributions vertical motion relative to the comet orbit plane and its implications to the tail structure. Arguments given in §2.5 yield two important results.One is a criterion to check the applicability of the FP(Finson and Probstein)-method.The other con- cerns with the somewhat peculiar structure to appears in the dust tail of comet after perihelion passage,which might be termed as《Neck-line structure(henceforce ab- breviated to NLS)》. In Part 3,we present a new interpretation of the anomalous tails refered to the concept of NLS.A discussion of the development of NLS is given,and it is shown that the emergence and development of NLS can provide an adequate expla- nation for the behaviour of the anomalous tail of C/Arend-Roland,1957 Ⅲ.Fur- thermore,statistical consideration on the visibility of anomalous sunward tail is at- tempted,the result of which also shows that the NLS-interpretation seems to be compatible with the data since 1801. In Part4,we develop a new method for numerical analysis of tail brightness. The basic idea of this method is to combine exact treatment of the motion of a large number of sample particles and counting-technique to estimate the surface brightness integral,taking account of the dust emission characteristics of comets which may be expressed by three source functions,namely,the emission rate N_d(t),the modified size-distribution f(γ;t),and the velocity distribution where Ψ(v;r,t)γ=1-μ). Distribution of tail brightness thus obtained gives essentially the exact solution for the assigned source funtions,in the sense that it is not affected by any auxiliary approximations.Moreover,no difficulties arise in the handling of source functions, because the requisite procedure can be reduced to the sampling of values of relevant parameters;thus the present method is applicable equally well for the case of ani- sotropic emission. In an application of the method for C/Arend-RolandPart4),we suppose that the emission rate varies as the inverse-square of heliocentric distanceN_d(t)∝[rc(t)]~(-2)), and that the velocity distribution is characterized as the isotropic one with a unique speed vo(t,γ).The function f(γ;t)is left as one to be determined through the comparison with observation. The function f(r)for C/Arend-Roland,derived by neglecting its time-dependency, is shown in Fig.16.The corresponding brightness probiles are compared with observed ones in Figs.14 and 15,for Apr.28 and Apr.30,respectively,it is worth noting that both main and anomalous tails have been treated in a unified manner, that is,without any temporal anomalies in emission characteristics. With these results,we conclude:(1)The simple forms presupposed for two functionsN_d(t)and Ψ(v;γ,t))may be well accepted as first approximations;(2) The derived function f(γ)shows its broad peak around γ=0.10~0.12 and possibly a secondary peak around γ~0.015;(3)The present brightness analysis adds support, in a quantitative way,to the NLS-interpretation of the.anomalous tails;(4)More observational data and careful analyses are needed,however,to establish the dust emission characteristics of comets.It is hoped that methods and viewpoints described in the present article may serve as the basis for future investigations.

本文以“三维的”粒子运动讨论了尘埃彗尾的结构,为了便于使用电子计算机和讨论各种μ值的粒子的运动,引入哈密顿积分 b,获得了以三维矢量和适用于各种μ值的开普勒运动的各个公式.考虑粒子的三维运动及其运动范围,使过近日点后的尘埃彗尾出现一“颈线结构”.利用此颈线解释向日尾并分析了其产生的可能性.最后给出了一种定量分析尘埃彗尾亮度分布的方法,本法的基本想法是在考虑有关粒子抛射的函数条件下,计算取样粒子的运动,并利用计数法求出其数密度.本文结果在所取函数条件下是一严格解.应用时,我们假定两函数N.(t_i),ψ(v;r,t)及 v_0的函数形式,以有关粒子性质的函数 f(r)为参量,分析了阿朗-罗兰彗星的尘埃彗尾(包括向日尾)的亮度分布(图14,15),并得到函数 f(r)(图16).

Many previous literatures considered that the operating frequency of an impulse governed oscillator (IGO) was difficult to be extended to the microwave band. One of the reasons put forward was that the width of the synchronizing pulse must be narrower than 1/5 to 1/3 of the period of the VCO, which was relatively difficult to achieve in the microwave band. Some recent literatures raised an objection to this, but still considered the narrower the synchronizing pulse for a microwave IGO in the case of non-ideal...

Many previous literatures considered that the operating frequency of an impulse governed oscillator (IGO) was difficult to be extended to the microwave band. One of the reasons put forward was that the width of the synchronizing pulse must be narrower than 1/5 to 1/3 of the period of the VCO, which was relatively difficult to achieve in the microwave band. Some recent literatures raised an objection to this, but still considered the narrower the synchronizing pulse for a microwave IGO in the case of non-ideal sample-and-hold, the better. This paper proves that neither of these conclusions is exactly true. In addition, previous literatures also doubted the loop stability of IGO, and held that its phase noise might be greater than that of a common phase lock loop. This paper discusses the problems concerning phase noise and loop stability. Theoretical analysis and an IGO experiment at 3GHz show that a correctly designed microwave IGO has low phase noise, better stability and a simpler, compact strip-line structure. Therefore further advances of the IGO may be expected.

过去许多文献认为,IGO环(脉冲锁相环,即脉冲控制振荡器的缩写)难以扩展至微波段,其理由之一是同步脉冲宽度必须窄于VCO周期的1/3—1/5,在微波段较难实现。近来,虽有文献对此论点表示异议,但仍认为微波IGO(非理想取样保持)的同步脉冲宽度愈窄愈好。本文指出了上述观点的不足之处。文中还讨论了IGO的相位噪声和环路稳定性等问题。理论分析和3GHz IGO的实验均证实,一个正确设计的微波IGO,确具相位噪声小、稳定性好、工艺简便,结构紧凑等优点。

Nova Cygni 1978 was observed from October 11 to December 23, 1978 at the Beijing Observatory with the grating spectrograph attached to the Naysmith focus of the 60/90-cm Schmidt telescope. This paper gives postmaximum photographic magnitudes, identification of the spectral features, emission line structures, intensity ratios of some emission lines and temperatures of the underlying star. The main spectral lines in wavelength range λλ3400—6700 from October 11 to 30 are those of the following...

Nova Cygni 1978 was observed from October 11 to December 23, 1978 at the Beijing Observatory with the grating spectrograph attached to the Naysmith focus of the 60/90-cm Schmidt telescope. This paper gives postmaximum photographic magnitudes, identification of the spectral features, emission line structures, intensity ratios of some emission lines and temperatures of the underlying star. The main spectral lines in wavelength range λλ3400—6700 from October 11 to 30 are those of the following atoms or ions: H, FeⅡ, NⅡ, TiⅡ, [0Ⅰ], [NⅡ], NⅢ. From November 10, lines of [OⅢ], HeⅠ and HeⅡ become visible one after another. The emission line H_α shows three components, of which the most redshifted is the strongest. In turn, each component consists of a number of weak emission peaks. Temperature of the underlying star increases with decline of the nova brightness. The upper limit of temperature may be~120000K.

本文给出新星极大后的照相星等m_(og)光谱成份、发射带结构、发射带相对强度比和核星温度。由10月11日至30日在3500—6700波长范围内它的主要光谱成份为H,FeII,NIITiII,[OI],[NII],NIII。从11月10日开始,陆续出现[OIII],HeI和HeII等谱线。H_a发射带由3个子峰构成,红移最大的子峰强度最大,每个子峰又各分成几个小子峰。核星温度随新星亮度的下降而升高,其温度上限可能为120000K左右。

 
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