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偏振     
相关语句
  polarization
    Polarization of Quasars: Electron and Resonant Line Scattering in the Broad Absorption Line Region
    类星体宽吸收线区的共振与电子散射偏振
短句来源
    OBSERVATION OF CIRCULAR POLARIZATION AT 3.2CM WAVELENGTH OF THE SOLAR ECLIPSE OF SEPTEMBER 22,1968.
    1968年9月22日日食的3.2厘米波段圆偏振观测
短句来源
    POLARIZATION OBSERVATION OF THE SOLAR CORONA AT THE SOLAR ECLIPSE OF 1968 SEPTEMBER 22.
    1968年9月22日日食的日冕偏振观测
短句来源
    Polarization Observations of 4 Southern Pulsars at 1560 MHz
    四颗南天脉冲星在1560 MHz上的偏振观测
短句来源
    Quick Reverse of the Polarization Sense of the Spikes and FFS Radiation
    SPIKES和FFS辐射偏振状态的快速逆转
短句来源
更多       
  polarized
    We present H and K s polarimetric images in a ~5′ field of star forming region NGC7538. The polarimetric images reveal the complex structure of infrared nebulosities and clusters of young stars, associated with the bright infrared sources IRS 1 11. The polarization pattern in the IRS 1 3 nebula shows a dominant illumination from deeply embedded source IRS 1. The morphology of the nebula can be modeled by a low extincted bubble enclosed by redder and highly polarized shell.
    介绍恒星形成区NGC7538的H和Ks波段偏振成像的观测结果.近5′视场的偏振图像揭示了与亮红外源IRS111成协的年轻星团和红外星云的复杂结构.IRS13星云的偏振图像表明星云的近红外辐射主要来自对深埋红外源IRS1的反射;
短句来源
    Observations and researchs of polarized spectra are basic methods to know the magnetic field in solar atmosphere and other remote stars.
    偏振光谱的观测和研究是我们了解太阳表面以及遥远天体上磁场的基本方法。
短句来源
    The basic physical principle of measuring magnetic fields、 the establishment of the polarized radiative transfer equation、 the solutions of the polarized radiative transfer equation and the inversion code of the magnetic fields are the main parts of this process.
    本文对太阳黑子磁场的观测分析过程进行了综述,主要分为,太阳磁场观测的物理原理、偏振Stokes参量辐射方程的建立、辐射转移方程的解、磁场测量的反演方法和太阳黑子矢量磁场分析。
短句来源
    The core of the active galaxy is known as Active Galactic Nuclei (ab.AGN), which has bright and dense nuclei, with polarized non-heat continuous radiation in radio, optical and X-ray band. There exists strong atomic and ionic emission, with the ability to send out more energetic photons than normal galaxies.
    活动星系核(Active Galactic Nuclei,简称AGN),有明亮的致密核区,在射电、光学、X射线波段存在偏振的非热致连续辐射,存在强的原子和离子发射线,具有比正常星系更强的发射高能光子的能力。
短句来源
    The reversal of polarized waves sense from type IV_u burst souree into type IV_(dm) source is explained by the fact that the direction of the magnetic field line in one source is anti-parallel to that in another.
    从Ⅳ_μ型爆发到Ⅳ_dm型爆发的偏振旋向反转是由于两个源中磁力线的反向平行所引起的。
短句来源
更多       
  polarisation
    POLARISATION ET COULEUR DU SPECTRE CONTINU DES NEBULEUSES GALACTIQUES
    銀河星雲的偏振和連續光譜的顏色
短句来源
    Deux cliches, correspondants a deux orientations de 1'analyseur differant d'un angle de π/4, suffisent pour determiner les pourcentages de lumiere polarisee et les directions des plans de polarisation de nombreuses aires nebulaires.
    在分析器(analyseur)的位置相差π/4所拍的兩張照片,就足以决定星雲各區偏振光的百分數和偏振面的方向。
短句来源
    Les resultats, identiques dans les domaines spectraux 4000—5000A et 5200—5800A, montrent une polarisation tres elevee (>40%), en accord avec la theorie developpee par Shklovsky et par Oort.
    據4000—5000埃和5200—5800埃兩光譜區所得的相同的結果,表現偏振度很强(>40%),這是和席克洛夫斯基(ShMovsky)与奧特(Oort)的理論相合的。
短句来源
    Les regions les plus polarisees montrent des taux de polarisation variant de 20% a 40% suivant les nebuleuses considerees.
    偏振化最强的區域,按所研究過的星雲,偏振度可由20%變至40%。
短句来源
    Si la polarisation radiale de NGC 7023 demeure le caractere principal de cette masse nebulaire, il semble mieux etabli que les directions des plans de polarisation observes coincident avec les trainees lumineuses decelables.
    如果NGC 7023的徑向偏振真是這團星雲物質的主要特徵,那么觀测到的偏振面的方向和可見的發光細絲相重合,更像是確定的事實了。
短句来源
  polarization properties
    Polarization Properties of Radio Pulsars in the Inverse Compton Scattering(ICS) Model
    射电脉冲星的偏振特性与逆康普顿散射(ICS)模型
短句来源
    In the second chapter we mainly present the basic observational properties,including the variability properties, polarization properties , radio structure and superluminal motion of blazars.
    第二章主要介绍了blazar天体的基本观测性质。 包括光变性质、偏振性质和射电结构及超光速运动性质。
短句来源
    Based on the works of Herold and us, we discuss the polarization properties of inverse Compton scattering in a strong magnetic field (both relativistic and non-relativis-tic cases). Some interesting results are obtained and compared with field-free condition.
    本文在Herold和我们前一工作的基础上,讨论了强磁场中不同情况(相对论情况和非相对论情况)下的逆Compton散射的偏振特性,并与无磁场情况进行了比较,得出一些有益的结果。
短句来源
    In research works on the mechanism of emission for those celestial bodies which emit X-ray and γ-ray in strong magnetic fields, or even those emit optical radiation only. These polarization properties should be considered.
    在研究气体,尤其是具有强磁场天体的高能X射线和γ射线,甚至光学辐射机制时,这些偏振特性必须给予充分注意。
短句来源

 

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      polarization
    In the interesting case when the group is of Coxeter typeDn (n≥4) we use higher polarization operators introduced by Wallach.
          
    When the characteristic of k is 0, it is known that the invariants of d vectors, d ≥ n, are obtained from those of n vectors by polarization.
          
    From elements of the invariant algebra C[V]G we obtain, by polarization, elements of C[kV]G, where k ≥ 1 and kV denotes the direct sum of k copies of V.
          
    The remanent polarization (Pr) and coercive electric field (Ec) of the measured PZT thin films are 47.7 μC/cm2 and 18 kV/cm, respectively.
          
    Impact of polarization mode dispersion and nonlinear effect on 40 Gbit/s dense wavelength division multiplexing system
          
    更多          
      polarized
    However, we show that the algebra of invariants is always the p-root closure of the algebra of polarized invariants.
          
    The liquid crystalline behavior of compound 3 was studied by polarized microscopy (POM) and differential scan calorimeter (DSC).
          
    Resolving the problem of cross sensitivity in fiber Bragg grating sensor based on the principle of polarized-light interference
          
    The article introduces an advanced approach of fiber grating strain demodulation based on the principle of polarized-light interference.
          
    As for the yttrium vanadate (YVO4) crystal polarized-light interferometer, if there are two different fiber Bragg gratings that have a π rad phase difference, one is used for strain sensor and the other is used for temperature compensating.
          
    更多          
      polarisation
    The temperature dependences of the intrinsic coefficients m113 and m333, defined in terms of the induced polarisation, are considered as well.
          
    Requirements for a pacemaker lead are: outstanding bio-compatibility, low pacing threshold, reliable sensing, high pacing impedance, low polarisation and corresponding longterm stability.
          
    The introduction of new electrodes with a porous or fractal surface led to a reduction in polarisation and therefore to an improved stimulation with regard to energy delivery.
          
    Das Korrosionsverhalten von neun verschiedenen orthodontischen Dr?hten wurde im Labor durch potentiodynamische Polarisation und durch Licht- und Rasterelektronenmikroskopie untersucht.
          
    Bei der potentiodynamischen Polarisation weisen diese Legierungstypen niedrige Durchbruchspotentiale von weniger als 600 mV sowie ein sehr ungünstiges Repassivierungsverhalten auf.
          
    更多          
      polarization properties
    We consider a taxonomic classification of gas and dust comets according to dust polarization properties.
          
    These were used to determine the integrated rotation measures of 18 sources, 15 of which had never been measured previously, which hindered analysis of the intrinsic polarization properties of objects in the complete sample.
          
    The polarization properties of radiation at the frequencies of resonance lines diffusely reflected from a scattering atmosphere are discussed.
          
    The polarization properties of a monochromatic beam of light are ordinarily determined by three numbers, for example, the Stokes parameters.
          
    The polarization properties of the effect are analyzed under various experimental conditions.
          
    更多          


    La polarisation des nebuleuses galactiques a ete observee en photographiant ces objets a travers un polarimetre de type Ohman ou Lyot. Deux cliches, correspondants a deux orientations de 1'analyseur differant d'un angle de π/4, suffisent pour determiner les pourcentages de lumiere polarisee et les directions des plans de polarisation de nombreuses aires nebulaires. Les mesures polarimetriques, effectuees sur la nebuleuse du Crabe, ont porte sur 29 aires de 8″ de diametre. Dans toutes les regions ou la structure...

    La polarisation des nebuleuses galactiques a ete observee en photographiant ces objets a travers un polarimetre de type Ohman ou Lyot. Deux cliches, correspondants a deux orientations de 1'analyseur differant d'un angle de π/4, suffisent pour determiner les pourcentages de lumiere polarisee et les directions des plans de polarisation de nombreuses aires nebulaires. Les mesures polarimetriques, effectuees sur la nebuleuse du Crabe, ont porte sur 29 aires de 8″ de diametre. Dans toutes les regions ou la structure filamenteuse de la masse "amorphe" n'est pas trop emmelee, les directions des plans de polarisation coincident avec celles des filaments decouverts par Baade (fig. 4). Les resultats, identiques dans les domaines spectraux 4000—5000A et 5200—5800A, montrent une polarisation tres elevee (>40%), en accord avec la theorie developpee par Shklovsky et par Oort. Malgre les difficultes d'observations des nebuleuses diffusantes en raison de leur faible luminance par rapport a celle du ciel nocturne, les mesures polarimetriques ont porte sur 117 aires appartenant a 10 nebulosites. Les regions les plus polarisees montrent des taux de polarisation variant de 20% a 40% suivant les nebuleuses considerees. Si la polarisation radiale de NGC 7023 demeure le caractere principal de cette masse nebulaire, il semble mieux etabli que les directions des plans de polarisation observes coincident avec les trainees lumineuses decelables. La polarisation trouvee pour les autres nebulosites ne peut etre qualifiee de radiale; mais il est encore possible de constater que la direction des plans de polarisation suit les trainees lumineuses les mieux definies. La determination des exces de couleur montre d'une maniere generale qu'une nebuleuse diffusante est un peu plus bleue que l'etoile qui l'eclaire, avec une variation systematique en fonction de la distance a 1'etoile. Les resultats des observations s'accordent avec ceux que donne la diffusion de la lumiere par des particules solides de dimensions comparables aux longueurs d'onde du spectre visible.

    銀河星雲的偏振曾經被人透過阿黑曼(Ohman)或李約(Lyot)的偏振計去做攝影觀測。在分析器(analyseur)的位置相差π/4所拍的兩張照片,就足以决定星雲各區偏振光的百分數和偏振面的方向。我們對於蟹狀星雲作了29個區域的偏振觀測,每個區域的直徑是8″。在那些“無定形”物質的纖維結構不太混淆的區域里,偏振面的方向和巴德(Baade)所發見的纖維的方向是相合的(圖4)。據4000—5000埃和5200—5800埃兩光譜區所得的相同的結果,表現偏振度很强(>40%),這是和席克洛夫斯基(ShMovsky)与奧特(Oort)的理論相合的。瀰漫星雲,因其光輝微弱並有夜天光陪襯,觀測是困難的;雖然這樣,我們在10個星雲的117區里,做了偏振的觀測。偏振化最强的區域,按所研究過的星雲,偏振度可由20%變至40%。如果NGC 7023的徑向偏振真是這團星雲物質的主要特徵,那么觀测到的偏振面的方向和可見的發光細絲相重合,更像是確定的事實了。有些星雲的偏振,不能說是徑...

    銀河星雲的偏振曾經被人透過阿黑曼(Ohman)或李約(Lyot)的偏振計去做攝影觀測。在分析器(analyseur)的位置相差π/4所拍的兩張照片,就足以决定星雲各區偏振光的百分數和偏振面的方向。我們對於蟹狀星雲作了29個區域的偏振觀測,每個區域的直徑是8″。在那些“無定形”物質的纖維結構不太混淆的區域里,偏振面的方向和巴德(Baade)所發見的纖維的方向是相合的(圖4)。據4000—5000埃和5200—5800埃兩光譜區所得的相同的結果,表現偏振度很强(>40%),這是和席克洛夫斯基(ShMovsky)与奧特(Oort)的理論相合的。瀰漫星雲,因其光輝微弱並有夜天光陪襯,觀測是困難的;雖然這樣,我們在10個星雲的117區里,做了偏振的觀測。偏振化最强的區域,按所研究過的星雲,偏振度可由20%變至40%。如果NGC 7023的徑向偏振真是這團星雲物質的主要特徵,那么觀测到的偏振面的方向和可見的發光細絲相重合,更像是確定的事實了。有些星雲的偏振,不能說是徑向的;但仍能證实偏振面的方向跟隨比較顯著的星雲亮絲。由色餘的测定,基本上表明:瀰漫星雲比較照耀它的星,更藍一點,這和星的距離的函数有系統的變化。觀测的結果和与可見光波長相近的固體質點對於光所生的漫射的情况,是相合的。

    This paper presents an analysis of the polarization characteristics of the radia- tion of the inner corona and its condensation region.Photographs of the corona were taken during the total solar eclipse of 22 September,1968 in the western part of Sinkiang. On the basis of analysis of the photographs with exposure 1/15 sec.the fol- lowing conclusions are drawn: About the inner corona:(1).In the range r≤1.54 R_⊙ the isophotes appear to be ellipses with rather small ellipticity.As for the variation of intensity...

    This paper presents an analysis of the polarization characteristics of the radia- tion of the inner corona and its condensation region.Photographs of the corona were taken during the total solar eclipse of 22 September,1968 in the western part of Sinkiang. On the basis of analysis of the photographs with exposure 1/15 sec.the fol- lowing conclusions are drawn: About the inner corona:(1).In the range r≤1.54 R_⊙ the isophotes appear to be ellipses with rather small ellipticity.As for the variation of intensity with r, the equator is brighter than the polar regions.(2).Except two local regions with angle of deviation from the radial direction Δф>10°,the direction of polarization of the inner corona approximately shows a radial regularity,with Δф<5°.In cer- tain regions the direction of polarization deviates from the radius with a common orientation.(3).The degree of polarization of the inner corona has a fine structure. Its value varies in the range 0.2—0.4,while anomalous polarization>0.6 can ap- pear in some local regions.Maximum degrees of polarization are attained at 1.35R_⊙ for the equatorial regions and at about 1.22R_⊙ for the polar regions,Their values are 0.42 at the east and the south and 0.35 at the west and the north. As regards the condensation region close to the east limb:(1).It occupies a range of about 28°,The maximum height above the limb is about 0.28R_⊙.Its total brightness is about three times brighter than the surrounding undisturbed corona. There is a horizontal shift in the cores of the isophotes of the condensation region. (2).The direction of polarization of the condensation region obviously has a re- gular deviation from the radial direction.The deviation angle lies in the range 15°—30°.(3).The degrees of polarization,simply treated with formula(4).lead to a very interesting result:The degrees of polarization on one side of the bright core of the condensation region are much larger than those of the surrounding un- disturbed corona,but on the other side we have just the opposite case.The mean degrees of polarization of the four regions are listed in Table 2. In the last part of this paper calculations of the electron densities have been carried out for 15 planes perpendicular to the radial direction.We have considered the mechanism of the electron scattering,assuming the following two models.(1). Two parts diffuse into each other.(2).Two parts have no mutual diffusion.The distribution of free electrons in the condensation region has been obtained.The maximum electron density in the center is about 7.7×10~9cm~(-3).

    本文介绍了1968年9月22日日全食的内冕和日冕凝聚区偏振观测方法及资料.在对内冕和东边缘凝聚区仔细分析的基础之上,得出如下结论:内冕:1)在小于1.54R☉范围内,内冕总强度的等强度线呈椭率较小的椭圆形,赤道亮于极区.2)内冕偏振度一般在0.2—0.4之间,偏振方向基本上呈现了径向性的规律,径向偏离角△ф<5°.东边缘凝聚区:1)东边缘凝聚区沿日面边缘延伸约28°范围,最大高度约达0.28R☉.2)凝聚区范围内的偏振方向与径向方向有一个较大的规律性的偏离,偏离角△ф在15°—30°之间.而且在其亮核的两边,凝聚区本身辐射的偏振度出现了特殊的变化规律.本文最后,还利用电子速度为零的散射机制,在两种模型的假设之下,计算了凝聚区的电子密度分布,最大电子密度达7.7×10~9cm~(-3).

    This paper gives a general description of the observation of circular polarization at 3.2cm wavelength of the solar eclipse on September 22,1968 and the main results obtained are: 1.As sunspots,bright knots and plages also have obvious circular polarization effect. 2.Our observation shows that the sunspot no.332 and the polarization source associated with it have one to one correspondence in nucleus-penumbra formation. Taking advantage of the characteristic high resolving power provided by solar eclipse observation,we...

    This paper gives a general description of the observation of circular polarization at 3.2cm wavelength of the solar eclipse on September 22,1968 and the main results obtained are: 1.As sunspots,bright knots and plages also have obvious circular polarization effect. 2.Our observation shows that the sunspot no.332 and the polarization source associated with it have one to one correspondence in nucleus-penumbra formation. Taking advantage of the characteristic high resolving power provided by solar eclipse observation,we have been able to resolve the double nuclei formation of that polariza- tion source,and attain the smallest separation between the double nuclei amounting to 2.″5. 3.It was observed that when the polarization source comes forth from behind the solar disk,the sense of circular polarization became reversed.

    本文叙述了紫金山天文台在1968年9月22日进行的日食观测中3.2厘米波段圆偏振观测的概况及计算、分析的结果。我们的观测得到日面各射电源的圆偏振流量密度、一维角径、非常波和寻常波的亮温度之差、磁场、偏振度、高度等参数(见总表)以及下列结果:1.不仅黑子,而且小亮点和谱斑都有明显的圆偏振效应。后两者的偏振流量密度和中、小黑子的偏振流量密度在同一范围。2.利用了日食观测的高分辨特性,观测到332号黑子与其上空的偏振源有一一对应的核——半影结构。并分解了该偏振源的双核结构,得到最小细节是2.″5角距离的核间半影。3.观测现象表明,偏振源从日面后转出时偏振波的旋转方向发生反转。

     
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