助手标题  
全文文献 工具书 数字 学术定义 翻译助手 学术趋势 更多
查询帮助
意见反馈
   尘埃 的翻译结果: 查询用时:1.219秒
图标索引 在分类学科中查询
所有学科
物理学
天文学
中国文学
外科学
气象学
预防医学与卫生学
地球物理学
更多类别查询

图标索引 历史查询
 

尘埃     
相关语句
  dust
     ≥ 0.5 μm dust 67 771.75 /L and 71 811.84 /L, decrease 5.63 %,χ 2 = 40.77 , P < 0.05 ;
     两组在燃烧过程中产生≥ 0 .5 μm尘埃粒子数 ,平均增量分别为 6 7771.75和 71811.84个 /L ,比对照组减少 5 .6 3 % ( χ2 =40 .77,P <0 .0 5 ) ;
短句来源
     RESULTS The elimination rate of the air bacteria,the small dust particle(≥0.5μm) and the big one(≥5.0μm) was 90.17%,29.43% and 90.42% at 20 min,respectively. But up to 1h there were 90.17%,52.63% and 94.64%,respectively.
     结果连续20min,空气中的细菌清除率达到90.17%,小颗粒尘埃(粒径为≥0.5μm)清除率为29.43%,大颗粒尘埃(≥5.0μm)则为90.42%,至1h,细菌清除率基本不变,但小颗粒与大颗粒尘埃分别提高到52.63%和94.64%。
短句来源
     The Analysis of ISO SWS Spectra and the Studies of Molecular and Dust Features for 29 SiC Carbon Stars
     29颗SiC碳星的ISO SWS光谱分析及其分子、尘埃特征研究
短句来源
     ≥ 0.5 μm dust as time going on was decrease, r = 0.988 8 , t = 11.47 , P < 0.05 ;
     尘埃粒子数随着点燃时间的延长而减少 (r =0 .9888,t=11.47,P <0 .0 5 ) ;
短句来源
     The results showed that in the filling workshops, the eligible rate of dust particles in air was 78.1%, that of total bacterial count was 81.3%.
     结果表明,灌装车间空气尘埃粒子合格率为78.1%,细菌总数合格率81.3%;
短句来源
更多       
  dust grains
     The temperature of dust grains, low temperature and high temperature ions and the number densities of the ions influence the property of dust acoustic waves.
     热尘埃等离子体中的非线性尘埃声孤波在高阶横向扰动下是稳定的,且尘埃颗粒的温度、低温离子和高温离子的温度和数密度影响尘埃声波的性质。
短句来源
     The dust grains have two kinds of motion: the pulse motion and the contrary cylinder center motion.
     数值模拟结果表明 ,尘埃颗粒随着调制磁场频率的改变 ,产生两种不同的运动方式 :pulse运动和除尘运动 .
短句来源
     And the dust grains carry up to 40% of the negative charges in the whole plasma.
     尘埃所带负电量与电机转速成正比 ,可达到等离子体负电量的 40 %。
短句来源
     The infrared emission of the complex is mainly caused by thermal equilibrium emission of standard dust grains.
     红外发射主要起源于标准尘埃粒子的热平衡发射。
短句来源
     Dust grains grow rapidly in the disks and gradually condense into planets, comets, and so on.
     在这种原始行星系统中间 ,尘埃颗粒逐渐生长 ,并凝聚成行星、彗星等 .
短句来源
更多       
  “尘埃”译为未确定词的双语例句
     Study of Interstellar Medium HC_ (3-x )NC_x (x=0~3) and HC_ 5-x NC_x (x=0~5) by Density Functional Theory
     星际尘埃HC_(3-x)NC_x(x=0~3)与HC_(5-x)NC_x(x=0~5)分子的DFT研究
短句来源
     In the sampled 200 homes, the proportion of homes with Dff F3 level of >10 μg/g was 57^0%, 29^5% for group of 2-10 μg/g, and 13^5% for group of <2 μg/g.
     检测200份家庭尘埃样品尘螨变应原,结果显示,Dff F3浓度>10μg/g的家庭占57.0%,2~10μg/g的家庭占29.5%,<2μg/g的家庭占13.5%。
短句来源
     The Optical Sensor in the Airbone Particle Counter for 0.1μm
     0.1μm 尘埃粒子计数器光学传感器
短句来源
     For radioactive ash contamination of skin, DF=57-1000 ( K =:98. 2%-99. 9%) in 4 h-delayed decontamination.
     对放射性尘埃造成的皮肤沾染,滞留4h后DF=57~1000(K=98.2%~99.9%)。
短句来源
     Infrared Radiation of IRAS/Cirrus Cloud 7
     IRAS/Cirrus7中的尘埃辐射
短句来源
更多       
查询“尘埃”译词为用户自定义的双语例句

    我想查看译文中含有:的双语例句
例句
为了更好的帮助您理解掌握查询词或其译词在地道英语中的实际用法,我们为您准备了出自英文原文的大量英语例句,供您参考。
  dust
The parameters considered are the applied high voltage U, the air flow F, and the quantity of dust in air m.
      
The Einstein gravitational equations in the spherically symmetric case and for the dust model (i.e., p = 0) have been studied by several authors.
      
In this case, the mixture area consists of abrasive dust from friction pairs, and the surface film is distributed with crumby hard granules, exiguous oxide, carbide granules and sheared slender fibre.
      
The values of optimal fiber radii are determined from the condition of maximal dust capacity of a filter at given limiting pressure drop and total initial efficiency.
      
On the Possible Existence of Radiation Dust Belts in Near-Earth Space
      
更多          
  mote
The band structure of α-MoTe2 by photoelectron spectroscopy
      
Vacuum-cleaved single crystals of α-MoTe2 have been investigated by photoelectron spectroscopy.
      
The increasing number of biomaterials for the skeletal system requires mote and move their distinct clinical application.
      
The most abundant fish larvae during this period were preflexion stage mote sculpins (Normanichthyidae) and newly hatched and preflexion stage anchovies (Engraulidae).
      
A second, smaller summer peak was dominated by preflexion stage anchovies, followed by preflexion stage mote sculpins.
      
更多          
  atomy
A review of the book Atomy legiruyushchikh primese
      
  dust grains
The density of the Galactic meteoroid background formed by the loss of large dust grains escaped from circumstellar disks during the formation of a star is estimated.
      
The temperature of nonspherical circumstellar dust grains
      
The temperatures of prolate and oblate spheroidal dust grains in the envelopes of stars of various spectral types are calculated.
      
Porous dust grains in the shells of Herbig Ae/Be stars
      
The masses and sizes of dust grains were estimated.
      
更多          
  其他


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...

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).

This article introduces a pneumatic bridge in adverse circumstances. The bridge may retain its equilibrium with variating supply, and free from block up while the measuring object is in a dusty environment and the supply is in a negative pressure.The va(?)iating supply cannot effect the equilibrium of the pneumatic bridge while the ratios of the exponents of the bridge-arms are equal. In addition, an alternating bias pneumatic bridge is designed to avoid block up.

本文研究的气桥在气源变动时,能维持其原来的平衡状态且当气源要求负压而被测物周围有许多尘埃时,能防止其堵塞。本文根据气阻的近似特性△p=KQ~m研究气桥的平衡,结果是:若气桥两臂的指数比相等,则气源的变动不会影响该气桥的平衡。为防止桥路堵塞,设计了一种特殊桥路——交流偏置桥路,已在实践中获得了成功的应用。

Arising from development of techniques in millimeter wave and infrared observatory, one can find a series complexes consist of HII regions-infrared sources-molecular clouds. W40 (G28. 8+3.5) is a complex which has already been detected by G. Westerhout, E. C. Reifenstein et al, H. Olthof and M. Zeilik et al. Basing upon these data we derived the basic physical parameters, we also calculated the cooling and heating rates for the gas and dust in W40. Finally we discussed the problems about the exchange and trasfer...

Arising from development of techniques in millimeter wave and infrared observatory, one can find a series complexes consist of HII regions-infrared sources-molecular clouds. W40 (G28. 8+3.5) is a complex which has already been detected by G. Westerhout, E. C. Reifenstein et al, H. Olthof and M. Zeilik et al. Basing upon these data we derived the basic physical parameters, we also calculated the cooling and heating rates for the gas and dust in W40. Finally we discussed the problems about the exchange and trasfer of energy among the component of W40 and the origin source.1. The physical parameters of the molecular cloud.Taking geometrical assumptions which had been used by J. Evans et al. As Fig 1 shows, an interior to a given contour level is the projected area of a sphere which has a radio ri=0.056 ai1/4, a surface area Si=4ai and a volume Vi=0.75 ai3/2. These regions are assumed to form a series of concentric shell with volume △Vi=Vi-Vi-1, each with uniform physical properties. The dimension of W40 is adopted 0.7 kpc.In collapsing cloud T=∞, Tk=Tex for the line of 12CO, so the kinetic temperature Tk (col. 3 of the table) can be directly derived from the antenna temperature TA* of 12CO.hereThe colum density of 13COn13L=5.6×1016/cm2. Using the formula nH2L==5.0×l05n13L for W40 we get the column density of H2nH2 L=2.8×1022/cm22. Taking L as the diameter of the sphere in which TA*=15 K we obtained nH2=6.7×103/cm3.From the empirical relation τFIR=10-18 n13 L, We find τFIR=0.056 at the centre of W40. Using the data reported by H. 01 thof we calculated the infrared luminosity in 20-200 μm band L20-200μm = 3.3×104L⊙.2. Energy transformation process of molecular clouds.We 11 respectively consider the two separate systems of gas and dust.(1) Energy relation for the gas.The cooling of H2 is primary through collision of CO with H2 molecular, in which energy is given to CO molecular, then it carried away out of cloud by emission of rotation line of CO molecule. Using the formula given by N. J. Evans we can calculate the. cooling rate of per shell of the contour map of W40 is (erg/cm2 ·s) and the total cooling rate of gas isFor the heating of the gas we consided two mechanisms which can supply it with the equal amount thermal energy with that carried away by CO emission. One is the collapse heating. From V(dE/dt)collapse= PheatingdV/dt and the expression of τff given by N.J. Evans we obtained that the temperature of W40 could maintain at 12.46 K.Another possible mechanism is the inelastic collision of dust with gas. The dust heated by the embeded infrared source transfers some energy to the gas in the collision. The supply energy efficiency of collision dust- gas may be represented by the collisionrelaxation time of dust-gas tr =1/vH,Ndσd Take criterion valuethus tr=4.5×1016NH2-1Tk-1/2s (here vH2 is mean thermal motion velocity of molecular hydrogen). This accords with expression by P. Goldreich and J. Kwan. As regards W40 central region tr=1.15×1012 s which is of the order just as τff. In the central region the cloud heated by dust just as it heated by collapse is rather primary mechanism.(2) Energy relation of dust.The dust in molecular cloud absorb the energy from the embeded IR sources, then they loss the energy by thermal radiation and by providing energy to gas. The balance between both keeps the dust is constant temperature.We derived the dust temperature of a shell in which the radius changes fromWhere the units of L and n are L ⊙ and pc respectively. For W40 the embeded sources emit infrared luminosity L is 3.3×104 L⊙ (Z-200μm), its Tdi is shown in column(6) of the table.There are two cooling mechanisms for the dust. One is the energy transters to gas by inelastic collisions of gas molecular and dust grains, as above, the total transferred energy Cdust-gas < 0.46L⊙. The another is the energy released by the thermal radiation of the dust. The power of thermal radiation is Ciradiation= σTd4Tisi, here si is the surface area of the shell, Ti is the mean optical depth of the shell through out fra-infrared

本文对W40(G28.8+3.5)中分子云的主要能量交换过程进行了研究。利用~(12)CO、~(13)CO分子谱线及红外观测资料,估算了W40中分子云的基本物理参数,并进而计算了它的气体冷却率、气体加热率、尘埃冷却率和尘埃加热率。并且通过对计算结果的分析,讨论了W40中分子云的气体、尘埃及嵌入红外源三者之间的能量制约关系。

 
<< 更多相关文摘    
图标索引 相关查询

 


 
CNKI小工具
在英文学术搜索中查有关尘埃的内容
在知识搜索中查有关尘埃的内容
在数字搜索中查有关尘埃的内容
在概念知识元中查有关尘埃的内容
在学术趋势中查有关尘埃的内容
 
 

CNKI主页设CNKI翻译助手为主页 | 收藏CNKI翻译助手 | 广告服务 | 英文学术搜索
版权图标  2008 CNKI-中国知网
京ICP证040431号 互联网出版许可证 新出网证(京)字008号
北京市公安局海淀分局 备案号:110 1081725
版权图标 2008中国知网(cnki) 中国学术期刊(光盘版)电子杂志社