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    For instance, what is the reason for the difference between the estimations of the oceanic tidal terms of EOP from real data reduction? How could the reliable time series of high frequency variation of EOP be solved from observation? What will be the effect of the modeling deficiency of precession and nutation on the solving of HF variation of EOP?
    例如,不同作者基于实测资料得到的EOP高频变化潮汐项估值存在差异的原因是什么,如何实测资料中得到更为可靠的EOP高频变化解算序列,岁差章动模型的缺陷对求解EOP高频变化有何影响等等。
短句来源
    Its basie ideas are the following 1. In our analysis, we adopt σ* as the fundamental elements system, where σ*'s are mean elements, obtained after subtracting the short, period terms △σ_s.
    这里σ~*是密切根数σ中扣去短周期项△σ_s的平根数。
短句来源
    After an analysis of the secular variation of the common Z-Term in latitude, the existence of the non-polar long period terms in latitude is verified.
    本文讨论纬度公共Z项长期变化的规律入手,证实了纬度非极变化中存在着某些长周期项。
短句来源
    In this paper some methods for the determination of the effective temperature of carbon stars are discussed in terms of their spectral and variable properties. Some results which arc derived from our recent infrared observations are compared with those previously obtained.
    本文仅碳星的光谱和可变特性出发,讨论了确定其有效温度的几种可能的方法,并将过去的一些结果与我们的观测所导出的结果进行了比较。
短句来源
    The CME event on May 6,1980,occurring between a pair of coronal streamers,is discussed in this paper. An empirical kinematical model is proposed for describing the motion of outer loop of the event,n which the observed profile of loop is fitted in terms of the Cassini function in a moving coordinate system. The development of the loop can be distinguished into two different phases.
    本文讨论了发生在冕流对之间的1980年5月6日日冕物质抛射事件.提出了一种描述事件外环运动的经验模型,把环的观测外形表达为在运动坐标系中的Cassini函数.环的发展过程分为两个阶段:在前一阶段,外环处于冕流对盔状结构之间,事件的发展以角宽度膨胀为主,其对称轴赤道向北纬方向移动;
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    Using the fine structure Ha-filtergram equipped at Guanyu station Purple Mountain Observatory, the compounding process of two active regions in Oct. 1990 is investigated. Because of the lack of simultaneously fine magnetograms, these Ha-filtergrams are analysied in terms of Zirin-Prata principle, with reference to Kitt Peak's magnetograms (S. G. D. data).
    本文用赣榆站所拍得的精细色球资料研究了1990年10月两个活动区的复合过程,在缺少适时准确的磁图条件下,我们以KittPeak磁图为背景,巧妙运用Zirin-Prata法则,剖析了此两区的发展过程。
短句来源
    In terms of different initial conditions, stable helical waves or irragular clouds may exist in different cometary tails.
    根据初始条件的不同 ,有的彗尾中可以产生稳定的螺旋波 ,有的则不然 ,只能是浑云状态。
短句来源
    Taking the total angular momentum conservation in place of tangential momentum conservation,and considering the square and higher power terms of orbital eccentricity e and effect of tidal interaction,the equations of changes of orbital elements of binaries are reduced for wind accretion scenario. These new equation of orbial elements are used to calculate the properties of barium stars,and compared the results with without tidal interaction.
    用整个系统的角动量守恒条件代替切向动量守恒条件 ,考虑轨道偏心率的二次以上的高次项和潮汐作用的影响 ,重新推导了星风质量吸积和轨道根数变化方程 ,在新的轨道根数变化方程的基础上计算了Ba星的星风质量吸积及轨道根数的变化 ,并和没有潮汐作用的情况作了比较 .
短句来源
  
    3. The osculating elements in computing dσ/dt are calculated with σ* plus the dt short period terms △σ_s, in which the first order short period terms △σ_s are obtained by analytical method, and the second order ones △σ_s by Fourier analysis.
    ii),计算dσ/dt中所用的密切根数σ,由σ~*加上短周期△σ_s,而得,其中一阶短周期△σ_s~((1))用分析公式计算,二阶短周期△σ_s~((2))用Fourier分析方法求取。
短句来源
    It is shown that the new results of general perturbations for those asteroids have been obviously improved because of considering (3E-10θ) long periodic term and refining the coefficients of main periodic terms including (E-3θ) term, etc.
    与过去用Bohlin群法计算所得近似解作比较,因现在计及了(3E-10θ)长周期和精化了(E-3θ)等主要周期的系数,使得这些小行星普遍摄动计算的结果有了明显的改进。
短句来源
    A total of 3986 active regions are recorded during the 21st Solar Cycle. We define 16(e. g. AR3804, AR4474)of the active regions as the strongest active regions in terms of 4 indicies —sunspot area, index of the X-Ray flares, 10.7cm radio flux and proton event index.
    太阳第21周实测到3986个活动区,以黑子面积、X射线耀斑指数、10.7cm射电爆发及质子事件等四指数,从中综合评估出AR3804、AR4474等16个最强烈活动区。
短句来源
    The Doppler broadening, Stark broadening and various kinds of broadening parameters of HeI 10830 A line in solar flare are calculated and discussed and consequently the following results are got: radiation damping can be neglected when compared with Doppler broadening, and in the case of generally accepted electron density in a solar flare (Ne= 3.2 ×1013 cm3 ), all the damping terms will not lead to distinguishable broadening in the HeI 10830 A profile.
    讨论了 HeI 10830A的 Doppler和 Stark加宽机制以及各种加宽参数的计算,并 得到以下一些结论:辐射阻尼对 HeI 10830 A的加宽作用与 Doppler效应相比可以忽略; 在公认的耀斑电子密度(Ne=3.2 ×1013cm-3)的情况下,所有阻尼均不可能产生可以 觉察的加宽;
短句来源
    When the higher-order terms are neglected, the 2PN equations of light ray reduce to the 1PX equations which widely appeared in many textbooks.
    当忽略掉更高阶的时,2PN光线方程将回到在很多教科书中广泛出现的1PN光线方程.
短句来源
  术语
    A STUDY OF FOUR TIME-RESORDING TERMS OF CHUJI,JIWANG,JISHENGPO AND JISIPO IN THE WESTERN ZHOU DYNASTY
    西周金文中纪时术语──初吉、既望、既生霸、既死霸的研究
短句来源
    It explains some terms and concepts in Almagest and cleared up their clue of historical development.
    4、对于《至大论》中出现的一些名词术语和概念及其发展的历史背景给予解释和澄清。
短句来源
    (2) analysis of every phase of the moon and the date when the phase can be observed corresponding to these terms ;
    (2)纪时术语的各种可能月相和日序的分析;
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  terms
We express them in terms of generatorsEij ofU(gl(n)) and as differential operators on the space of matrices These expressions are a direct generalization of the classical Capelli identities.
      
In particular, we give a detailed description of these sets in terms of cross-sections inside maximal R-tori ofH.
      
A characterization of the complexity of a homogeneous space of a reductive groupG is given in terms of the mutual position of the tangent Lie algebra of the stabilizer of a generic point of and the (-1)-eigenspace of a Weyl involution of.
      
Indeed, we will give a full classification of the manifoldsN(g, V) which are commutative spaces, using a characterization in terms of multiplicity-free actions.
      
It was then observed independentely by Lusztig and Ginzburg-Vasserot (see [L1], [GV]) that this construction admits an affine analogue in terms of periodic flags of lattices.
      
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By introducing the non-dimensional variables defined by = (n + 1) (1 - θ) and ζ=|1+n|~(1/2)ξ,a generalized Lane-Emden equation of index n is obtained, which is applicable for any value of n (including the isothermal case), except in the case of constant pressure, n=-1. The solutions are then discussed in terms of the characteris- tics of the singular points on the (u, v)-plane. From the study of the stability against the radial perturbations, a condition of instability is derived. With this criterion,...

By introducing the non-dimensional variables defined by = (n + 1) (1 - θ) and ζ=|1+n|~(1/2)ξ,a generalized Lane-Emden equation of index n is obtained, which is applicable for any value of n (including the isothermal case), except in the case of constant pressure, n=-1. The solutions are then discussed in terms of the characteris- tics of the singular points on the (u, v)-plane. From the study of the stability against the radial perturbations, a condition of instability is derived. With this criterion, we can transform the stability problem into a geometrical discussion. For Emden solu-tion, the whole range of n is divided into the stability region, the thermal and gravita-tional instability regions (fig. 5b).

本文利用变数ψ=(1+n)(1-θ)和ζ= |1+n|~(1/2)ζ求得Lane-Emden方程的一般形式,此式适用于n=-1以外的所有多层体指数。对三种对称几何形状,用(u,v)面上的奇点性质讨论了n在整个数轴(-∞

In this paper a new semi-analytical and semi-numerical method for computation of the second order perturbation of artificial earth satellites is presented. Its basie ideas are the following 1. In our analysis, we adopt σ* as the fundamental elements system, where σ*'s are mean elements, obtained after subtracting the short, period terms △σ_s. from the oscula-ting elements. 2. The σ*'s secular and long period rates (up to third order) are derived with the numerical averages of dσ/dt, which are the rates...

In this paper a new semi-analytical and semi-numerical method for computation of the second order perturbation of artificial earth satellites is presented. Its basie ideas are the following 1. In our analysis, we adopt σ* as the fundamental elements system, where σ*'s are mean elements, obtained after subtracting the short, period terms △σ_s. from the oscula-ting elements. 2. The σ*'s secular and long period rates (up to third order) are derived with the numerical averages of dσ/dt, which are the rates of the osculating elements. 3. The osculating elements in computing dσ/dt are calculated with σ* plus the dt short period terms △σ_s, in which the first order short period terms △σ_s are obtained by analytical method, and the second order ones △σ_s by Fourier analysis. Because of adopting σ~* as the elements system, we have overcome some shortco-mings in the numerical method, such as the shorter step, the longer computing time, the more serious accumulatation of errors, etc. As we compute dσ~*/dt and △σ_s by means of numerical method, we have avoided the development of the complicate for-mulae. In this way, our method also has the advantages of simpler computing for-mulae and more convenient programming. To compute the second order perturbation, the computing time of our method is only 1/10 of the classical numerical method, and the memories is about 1/5 of the pure analytical method. The numerical method of ODE are also discussed. An improved Chebychev itera-tion process is developed to adapt the need of the orbit determination in satellite dynamical geodesy. In this paper we also give detailed formulae for computing the perturbating forces and the numerical results of computation by our method. The numerical results show that the errors in radius and across-track are less than 0.1 m, and that in along-track less than 1 m.

本文提出了一种新的计算人造卫星二阶摄动的半分析、半数值方法,其基本思想是: i),采用σ~*作为基本根数系统;这里σ~*是从密切根数σ中扣去短周期项△σ_s的平根数。 ii),σ~*的长期、长周期变率(准到三阶)由密切限的变率dσ/dt的数值平均求得。 ii),计算dσ/dt中所用的密切根数σ,由σ~*加上短周期项△σ_s,而得,其中一阶短周期项△σ_s~((1))用分析公式计算,二阶短周期项△σ_s~((2))用Fourier分析方法求取。由于采用了σ~*作为根数系统,克服了密切根数σ数值方法的积分步长短、计算时间长、积累误差大等缺点;由于dσ/dt、△σ_s~((2))用数值方法计算,又避免了繁复的公式推导,兼得了计算公式简单,程序编制方便等优点。用本方法计算二阶摄动,计算时间比经典的数值方法要节省十分之九,所占内存的大小可比分析方法节省4/5—5/6。本文还讨论了微分方程的数值积分方法,改进了迭代过程,使得它更适合于卫星动力测地中测轨的要求。本文还给出了用本方法计算的数值结果。数值结果表明:用本方法测轨,向径、垂迹方向误差小于0.1米,沿迹方向误差小于1米。

This paper deals with the steady basic state of disk galaxy with finite thickness. A hydrodynamical model is adopted. In terms of the small parameterε=8/R, the solutions in zero’th order and first order of approximation are obtained. These results will be used in the further studying 3-dimensional density wave of disk galaxy. In the appendix the general analytical solution of Poisson’s equation is derived.

本文从流体动力学模型出发,引用星盘曲线坐标系,求解了有限厚度盘状星系的三维基态,在薄盘条件(ε<1)下,求得了零级近似、一级近似的解析解,过程十分简明。在附录中,给出了一般的非对称的泊松方程解式。

 
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