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galactic halo
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  银晕
    Calculating the chemical evolution of galactic halo with Miller-Scalo initial mass function
    利用Miller-Scalo初始质量函数计算银晕的化学演化
短句来源
    In the last section of this paper, we calculate and discuss the probability todetect FGS using the chemical evolution model of Galactic halo posed by Tsujimotoet al (TSY99) under the assumption that the first generation of star has Miller-Scabform of initial mass function .
    本文最后部分根据Tsujimoto等人提出的TSY银晕化学演化模型,并假设形成第一代恒星的初始质量函数具有Miller-Scalo的形式,从理论上预言和讨论探测第一代恒星的可能性。
短句来源
    Galactic halo is an important composition of the Galaxy. This paper calculate and discusses the chemical evolution of the early Galactic halo with Miller scalo initial mass function and TSY model by fitting the count of the halo stars with different metal abundance to observations.
    银晕是银河系的重要组成部分 ,本文利用 Miller-Scalo形式的初始质量函数并结合 TSY化学演化模型 ,通过拟合晕族恒星随金属丰度的计数的观测值 ,对早期银晕的化学演化的一些特征进行计算和讨论
短句来源
    We calculate and discuss the probability to detect FGS using the chemical evolution model of Galactic halo posed by Tsujimoto et al (TSY 99) under the assumption that the first generation star has Miller Scalo form of initial mass function.
    为解释这一观察现象 ,将以Tsuiimoto等人提出的银晕的化学演化模型为基础 ,假设形成第一代恒星的初始质量函数具有Miller Scalo的形式 ,从理论上预言和讨论探测第一代恒星的可能性 .
短句来源
    We also describe the basic principle of white dwarf cosmochronology and its application in defining the age of the Galactic disk, globular clusters, open clusters and Galactic halo.
    介绍了白矮星宇宙纪年学研究的基本原理及其在银盘、球状星团、疏散星团以及银晕年龄确定方面的应用现状。
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  “galactic halo”译为未确定词的双语例句
    They showthat the distribution of the gamma-ray burst sources is isotropic but nonuniform, andindicate that the bursts located at either the extended galactic halo or the cosmologicaldistance.
    观测表明,γ暴源的空间分布是各向同性但不均匀的。
短句来源
    The parameter of model are confined by the observational data of the Galactic halo stars.
    利用已有的晕星的观测资料限定模型的参数 .
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  galactic halo
It appears to be relatively easy to account for up to approximately 10% of the galactic halo dark matter via SVT theories of gravity.
      
Constraints to the radiative lifetime of a light neutral fermion in the galactic halo from IUE
      
We review the distribution of diffuse gas, both neutral and ionized, in the Galaxy and the galactic halo.
      
An analysis of EGRET data has led to the discovery of a statistically significant diffuse γ-ray emission from the galactic halo, which turns out to be in remarkably good agreement with our prediction.
      
Basically, cosmic-ray protons in the galactic halo scatter on the clouds clumped into dark clusters, giving rise to a γ-ray flux.
      
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According to the principle and procedures presented in ref. [4], we have identified and analyzed the absorption lines spectrum of QSO OQ172 (=PKS 1442+101, Zem = 3.543) obtained by Chen et al., and found such a redshift system as shown in Table 1.There are 9 lines in this system, and 5 of which are Lα-L∈ of neutral hydrogen with equivalent widths consistent with the astrophysical constrains. The rest four lines are SiⅡ1260.42, NⅡ 1083.99, OVⅠ 1031.94 and FeⅡ1144.95. Their identifications are not reliable owing...

According to the principle and procedures presented in ref. [4], we have identified and analyzed the absorption lines spectrum of QSO OQ172 (=PKS 1442+101, Zem = 3.543) obtained by Chen et al., and found such a redshift system as shown in Table 1.There are 9 lines in this system, and 5 of which are Lα-L∈ of neutral hydrogen with equivalent widths consistent with the astrophysical constrains. The rest four lines are SiⅡ1260.42, NⅡ 1083.99, OVⅠ 1031.94 and FeⅡ1144.95. Their identifications are not reliable owing to the lack of other strong components of each multiplet and likely resulted by chance (see ref. [6]).By using the method showed in refs. [4] and [6], the statistical test for the five hydrogen lines has been made. Counting the number of the experiments n (=2021) and taking n, B, μ and u defined by eqs. (2)-(7) (using the same symbols of refs. [4] and [6]), we obtained the u-value =9.748 which is much greater than u0≈1.645, the rejection region for the significant level α=0.05, and even greater than u0≈2.35 for α=0.0.1.The result for S=98.9, the signal-to-noise ratio for the redshift system in question, is much greater than S (≈3.5), the mean value of those for all candidate systems in OQ172's spectrum, see eq. (8).For the five lines Lα-L∈, we have adopted the curve of growth for a single Maxwell velocity distribution and deduced Doppler widths b=55Km S-1 and column density of hydrogen lgNH=14.66 on the assumption there is no broadening by damping. The values (if IgWλ/λ and Igfλ of these lines are listed in the last two columns of Table 1.Our conclusion are as follows: the redshift system with 2=3.35248 is a reliable pure-hydrogen one. It can not be caused by any galactic halo, which has more complex, chemical composition. The absorber we have detected should be a primitive hydrogen cloud. On the basis of the Friedmann cosmological model, put q0=0.5, we have got the age of this cloud to be 0.11 of the Hubble time, see eq. (9).

根据对类星体OQ172吸收线光谱的证认,可靠地确定了一个由氢线(L_a~L_b)支持的红移系统z=3.35248,分析表明它是一个大爆炸后形成的原始氢云。假定不存在阻尼加宽,用生长曲线求得其柱密度 lgN_H=14.66,多普勒宽度 b=55km/s。

We have introduced the recent observational results obtained by the burst and transientsource experiment(BATSE) on the Compton Gammaray Observatory. They showthat the distribution of the gamma-ray burst sources is isotropic but nonuniform, andindicate that the bursts located at either the extended galactic halo or the cosmologicaldistance. Then, we have discussed the models about the origin of gamma-ray bursts,including the neutron star merging model and black hole accreting model etc.. Finally,we have...

We have introduced the recent observational results obtained by the burst and transientsource experiment(BATSE) on the Compton Gammaray Observatory. They showthat the distribution of the gamma-ray burst sources is isotropic but nonuniform, andindicate that the bursts located at either the extended galactic halo or the cosmologicaldistance. Then, we have discussed the models about the origin of gamma-ray bursts,including the neutron star merging model and black hole accreting model etc.. Finally,we have also discussed the possibility that there may be two different kinds of gammaraybursts.

介绍了ComptonORO卫星对γ暴的最新观测结果。观测表明,γ暴源的空间分布是各向同性但不均匀的。这种分布基本上排除了γ暴起源于银盘内中子星的模型,表明γ暴要么位于展延的银晕里,要么位于宇宙学距离上。我们讨论了目前关于γ暴起源的各种理论模型,包括两个中子星相撞、黑洞吸积等。最后还分析了存在两种不同类型γ暴的可能性。

Globular clusters are ones of the most ancient objects in the Galaxy. They are very important tracers in the Galactic halo due to their high accumulated luminosity. Today, about more than 140 globular clusters in the Galaxy are observed. Radial velocities of 120 globular clusters within galactocentric distances R<40kpc are accurately determined. These globular clusters can be subdivided into some groups based on their radial velocities and metallicities. Up to now, only 38 globular clusters' absolute proper...

Globular clusters are ones of the most ancient objects in the Galaxy. They are very important tracers in the Galactic halo due to their high accumulated luminosity. Today, about more than 140 globular clusters in the Galaxy are observed. Radial velocities of 120 globular clusters within galactocentric distances R<40kpc are accurately determined. These globular clusters can be subdivided into some groups based on their radial velocities and metallicities. Up to now, only 38 globular clusters' absolute proper motions are determined. The accuracy of these Values is much lower than that of the radial velocities and distances. Using these data above, however, some interesting results have been attained from the three-dimensional space motions of these globular clusters. At present, it become possible to determine the absolute proper motions of globular clusters based on the International Celestial Reference name, optically represented by the new reference frame established by Hipparcos. It is of importance for the study of space motions of globular clusters and of the structure and earlier evolution of the Galaxy.

球状星团是银河系中最古老的天体类型之一,其累积光度很大,是银晕中重要的示踪天体。已经发现的银河系球状星团有140多个,其中120个银心距 R< 40 hpc的星团已被准确地测定了视向速度。根据这些数据以及球状星团金属度的统计分析,可以把球状星团次系再进一步分成某些不同的族群。目前已经测定过绝对自行的球状星团只有38个。尽管这些自行的精度比视向速度和距离的精度差很多,然而,由此可以得出三维的空间速度,在统计上显露出一些很有意义的结果。Hipparcos星表的建立,将有可能把球状星团自行的测定直接建立在这一星表所体现的国际天球参考架之上,使得对球状星团空间运动的研究具有更坚实的基础,为银河系结构和早期演化研究作出更重要的贡献。

 
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