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色指数     
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  colour index
     A STATISTICAL ANALYSIS FOR QUASARS WITH RADIO COMPONENTS STRUCTURE Ⅱ.RELATIONS OF ABSOLUTE VISUAL MAGNITUDE,ABSOLUTE RADIO MAGNITUDE AND COLOUR INDEX DIFFERENCE Q WITH THE LINEAR DISTANCE BETWEEN COMPONENTS,AND THE ASSOCIATED EVOLUTION FEATURE
     有射电子源结构类星体的统计分析 Ⅱ.绝对视星等、绝对射电星等和色指数差Q与子源线距的关系以及有关的演化特征
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     3.The colour index difference Q decreases with the increase of D.
     3.随着子源间线距D的增大,色指数差Q下降.
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     They are given in Table 5. By the analysis of the correlation between the residuals and the terms with magnitude or colour index, it will not be necessary to take these terms into account for the plate reduction, if the size of configuration and the magnitudes and colour indexes of the reference stars are restricted to a certain range and the plates are taken around the meridian and in small zenith distances.
     残差与带有星等或色指数的诸项之间相关系数的分析判明,只要对定标星的位形大小以及星等和色指数范围作较严格的限制,而且在中天附近天顶距不太大的情况下摄取底片,归算时就可以不考虑这些项的影响。
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     This paper shortly introduce recent advance on two problem: occurrence of organic matter (only dispersed but heterogeneous) and new maturity indator-Transmittance Colour Index (TCI) in the carbonate source rock study.
     简要介绍了碳酸盐源岩研究中的两个问题:有机质的赋存状态(分散且不均一)及确立成熟度的新指标透射色指数(TCI)的最新进展。
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     Observed results show significant rapid variation and exhibit short-time variability of 23 min in R band. It is found a strong correlation between the B-V colour index and the magnitude in the B band. CCD photometry of H0323+022 showed that they are in good agreement with the results of Bai et al (1998).
     色指数B—V与V波段的星等值有较强的相关性,对H0323+022CCD测光的结果与Bai(1998)观测的结果ΔR=0.63ΔI=0.81是一致的.
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  color index
     But the statistics analysis show the distrbution of corona activity of late type with color index and rotation period exist upper limit.
     演化恒星的磁冕球活动在色指数和自转周期的分布上都显示出冕球磁活动存在上限的现象,并且对冕球磁活动上限的拟合表明在色指数B一V为1.0附近和自转周期!
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     By the reserching the relation between stellar chromospheric activity and color index, we find that stellar ages play a pivotal role for producing Vaughan-Preston gap of MS stars.
     通过主序星的色球活动对恒星色指数不同依赖关系的研究,我们分析了Vaughan—Preston间隙产生的原因,分析结果显示恒星的年龄在这一间隙的形成中扮演了重要的角色。
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     Infrared photometry in J, H and K bands of 24 carbon stars in The Galaxy is presented in this paper. The distribution of these carbon stars in the (J-H)-(H-K) color index diagram is described, and the bolometrie corrections along with the absolute bolometric magnitudes are given as well.
     本文给出了银河系24颗碳星的JHK波段的测光结果,文中时论了碳星在(J-H)-(H-K)双色指数图上的分布。
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  color indices
     Long Period Variability and Color Indices Variability of 0716+714
     0716+714的长期光变和色指数变化
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     Both color indices decrease along the Hubble sequence, but dispersion of color is very large. Averaged according to morphologicaltype,(B-V)_T~o ranges from 0.87 for E galaxies to 0.35 for I_m galaxies;
     沿哈勃序色指数逐渐减小,即颜色变兰,但弥散度很大,按类型平均,(B-V)_T~O从E系的0.87到I_m系的0.35;
短句来源
     Both color indices decrease along the Hubble sequence, but dispersion of color is very large. Averaged according to morphologicaltype,(B-17)_T~o ranges from 0.87 for E galaxies to 0.35 for I_m galaxies;
     沿哈勃序色指数逐渐减小,即颜色变兰,但弥散度很大,按类型平均,(B-V)_T~O从E系的0.87到I_m系的0.35;
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     Study on the Relationships of Color Indices for Blazar
     Blazar色指数相关研究
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     The associated infrared source IRAS19282+1814 may be a massive young stellar object (YSO), which is embedded in the surrounding gas and dust according to the IRAS color indices.
     它的成协红外源IRAS19282+1814可能是大质量年轻星体,其IRAS波段色指数表明该源深埋于气体和尘埃物质之中. 由60-100μm流量密度获得尘埃温度为30K.
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  chromatic index
     A new upper bound of the strong chromatic index
     强色指数的一个新的上界
短句来源
     In order to determine whether exist chromatic index critical graph of order 14, we should determine chromatic index critical of order 13 at first.
     要想确定是否存在14阶色指数临界图,首先需要确定出13阶临界图的结构和特征。 这篇论文的主要目的就是确定所有的13阶色指数临界图。
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      colour index
    A haemolymph colour index is developed in an attempt to improve the resolution of serum protein data in the characterisation of temporal and spatial changes in the condition and growth of a wild population of Jasus edwardsii.
          
    Indeed, male visit rate increased with their bill colour index independently of age, and brood condition was higher for adult males, compared to yearlings, independently of bill colour.
          
    The majority of samples have a limited range ofδ18O values (+10.0-+10.4) that is anticorrelated with colour index; this variation is compatible with crystallization of rocks with varying mineral abundances from an homogeneous (for oxygen) reservoir.
          
    By applying the zenith-sky colour index technique, which works under most weather conditions, the data availability can be extended.
          
    In general, colour index-effective temperature calibrations for carbon stars are quite different from those for K-M giant stars.
          
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      color index
    The u-x color index, which is related to the position of the absorption band at 950 nm in the asteroid spectra, was chosen for a qualitative comparison of the surface composition of these asteroids (identical or differing composition).
          
    For the first time, the phase-angle dependence was obtained for the color of the dust of comet Halley: the color index BC-RC systematically decreases with increasing phase angle.
          
    The analyzed characteristics included: O2, H2S, CH4, microelements; mineral and organic compounds of P and N, ionic composition components (HCO3-, Cl-, Na+, K+, dry residue, pH; color index, electrical conductivity.
          
    Possible variations (up to 27%) in the salinity and color index of MWM in years with different genetic composition are demonstrated and shown to be attributable to different water abundance in these years.
          
    The parameters of this law for turbidity, color index, permanganate oxidability, and ammonia concentration are evaluated.
          
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      color indices
    The color indices B-V and V-R showed no noticeable variations with this period.
          
    We performed a frequency analysis of the B-V and V-R color indices and the V magnitudes based on data averaged over five measurements, which provided an accuracy of the mean color indices and magnitudes of ~0.m005 and 0.m08, respectively.
          
    Our analysis of the color indices showed the absence of the known period, 0.d3405 (8.h172), and the presence of several periods at a confidence level of 7-10 σ, including P0 = 2.h93 (1/P = 8.17c/d) and its alias 2.h64 (1/P = 9.17c/d).
          
    The analysis of the synthetic values of the color indices determined from the spectrophotometric observations in 2000 confirmed the presence of quick spectral variations.
          
    The observed J-K and K-L color indices for both symbiotic novae, while decreasing, tend to the values typical of Miras.
          
    更多          
      chromatic index
    The minimum number of colors needed tofg-color a multigraphG is called thefg-chromatic index ofG.
          
    Various upper bounds are given on thefg-chromatic index.
          
    One of them is a generalization of Vizing's bound for the ordinary chromatic index.
          
    Our proof is constructive, and immediately yields a polynomial-time algorithm tofg-color a given multigraph using colors no more than twice thefg-chromatic index.
          
    We establish a minimax formula for the chromatic index of series-parallel graphs; and also prove the correctness of a "greedy" algorithm for finding a vertex-colouring of a series-parallel graph.
          
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    Basic quantities in stellar photographic photometry (in particular, colour index and "effective wavelength") are formulated according to the assumptions that: 1) stellar radiation may be represented by some black body equivalent and 2) within the limits of a single photometric "receiver", intensity-wavelength relationship of the radiation may be taken as linear. Foundations and applicability of these assumptions are examined. On the basis of this the photometric side of the problems of space reddening etc. are...

    Basic quantities in stellar photographic photometry (in particular, colour index and "effective wavelength") are formulated according to the assumptions that: 1) stellar radiation may be represented by some black body equivalent and 2) within the limits of a single photometric "receiver", intensity-wavelength relationship of the radiation may be taken as linear. Foundations and applicability of these assumptions are examined. On the basis of this the photometric side of the problems of space reddening etc. are discussed. We considered in detail the use of effective wavelength by objective grating method in stellar photometry and have shown that with suitable photometric technique and right choice of grating it is possible to obtain in two colour photometry (say, ultraviolet and photovisual) the results with same degree of accuracy as might be obtained in three colour arrangement.

    本文對着當前的發展,綜述了照相方法在恆星光度学中的地位.接着用兩個簡單的假设,即星体幅射的黑體近似和累積亮度範圍中的直线近似,把恆星光度学中的基本定義(如有效波長、等光波長和色指数等)和主要问题(如空間红化,亮度效应等)表以公式.在进行的時候,我们详细地讨论了這兩个假设的依據. 我們提出了在兩色光度学中物端光栅所能接觸到的问题,着重地敘述了空间吸收和光度型的辨認,並且把应用这种方法的先決條件,它的優點和它所受到的限制加以讨论.

    The star no. 1082 in Kustner Catalogue of M15 is a new type variable. Its period is 0.087 004 and amplitude is about 0.2. It has a B-V color index +0.10. This makes its position on the color magnitude diagram go out of the hot border of δ Scuti stars. We classify it temporarily as a hot ultrashort period Cepheid. So the hot Cepheids may be a sub-type of the Population Ⅱ ultrashort period cepheids.

    球状星团M15里的K1082星,是一颗新型的变星。这颗变星的周期是0~d.087004,变幅约为0.2等。它的光变曲线具有缓长的上升段和快陡的下降段。它的B-V色指数约为+0.10.其在颜色星等图上的位置,处在盾牌座δ型星的热边界的左外。它可能属于人们正在探寻讨论中的星族Ⅱ超短周期造父变星的一个次型,我们暂称之为热超短周期造父变星。

    Based upon our first paper and continuing the "Standard candle" classification by use of the component linear distance D, we attain to the following statistical correlation of some type of Quasars with largest angular diameter Q_(max): the correla- tion between visual magnitude and redshift; the correlation between its absolute magnitude, radio-luminosity of single frequency, integral radio Iuminosity, colour in- dex difference Q and D. According to these statistical laws, a series of inferrences on the evolution...

    Based upon our first paper and continuing the "Standard candle" classification by use of the component linear distance D, we attain to the following statistical correlation of some type of Quasars with largest angular diameter Q_(max): the correla- tion between visual magnitude and redshift; the correlation between its absolute magnitude, radio-luminosity of single frequency, integral radio Iuminosity, colour in- dex difference Q and D. According to these statistical laws, a series of inferrences on the evolution prop- erties have been derived as follows: 1. The optical luminosity decreases with the increase of D. dM_v/dD=10.~m6/MPC. 2.The radio luminosity decreases with the increase of D. dM_(4,8-5000)=9.~m17/MPC. 3.The colour index difference Q decreases with the increase of D. dQ/dD=-1.~m55/MPC. 4.In the process of evolution, radio spectral type, defined by the spectral in- dex, does not change in general. 5. Optical radiation is mainly lion-thermal, but thermal radiation increases gra- dually with evolution. 6.The time scale estimated from optical luminosity, radio luminosity and col- our index difference Q, all have nearly the same value, 1.6 10~7 yr. 7. There is no discrepancy between the above features and the viewpoint that QSO_s evolve to galaxies. 8.There is no apparent statistical dependence between D and the distance, i. e. no evidence to, imply that all QSO_s were formed at the same epoch. This is con- trary to the views of the bigbang cosmology.

    本文在第I部分的基础上,继续用类星体射电子源线距D进行“标准烛光”分类,经过统计分析,得到了子源角径最大的一类类星体的一些统计规律:它的视星等与红移之间,它的绝对星等、单频射电光度、积分射电光度和色指数差Q与D之间有很好的相关性等.由此得到下列有关有子源类星体演化性质的推论:1.随着子源间距D的增大,光学光度下降:dM_v/d_D=10.~m6/MPC.2.随着子源间线距D的增大,射电光度下降.dM_(408-5000)/dD=9.~m04/MPC.3.随着子源间线距D的增大,色指数差Q下降.dQ/dD=-1.~m55/MPC.4.在演化过程中,射电谱型,即谱指数基本保持不变.5.光学辐射主要是非热致的.但随着演化,热致辐射的成分渐渐增多.6.根据光学光度、射电光度以及色指数差Q三种物理量所估计的类星体的演化时标基本一致,大约是1.6×10~7年.7.这些性质和类星体最后演化为星系的总观点不矛盾.8.子源线距D与距离间没有明显的统计相关,即没有迹象表明类星体是在同一个时代产生的,这是大爆炸宇宙学所不能解释的.

     
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