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
   star formation 的翻译结果: 查询用时:0.156秒
图标索引 在分类学科中查询
所有学科
天文学
更多类别查询

图标索引 历史查询
 

star formation
相关语句
  恒星形成
     Star Formation Properties of Galaxy Cluster Abell2255
     星系团Abell2255的恒星形成性质
短句来源
     OBSERVATIONAL STUDY OF H_2O MASER IN THE STAR FORMATION REGION
     恒星形成区H_2O对脉泽的观测与研究
短句来源
     The star formation properties of 184 galaxies in the galaxy cluster Abell 2255 are studied.
     研究了星系团Abell 2255中184颗成员星系的恒星形成性质.
短句来源
     It lies at a distance of 1.4kpc, and its average reddening of E(B-V) is 0.47. It provides an excellent sample for the study of star formation and their early evolution.
     该星团离我们的距离约为1.4kpc,红化值E(B-V)约为0.47。 它经常被用来研究恒星形成和早期演化。
短句来源
     Molecular Clouds in Different Evolutionary Stages and Star Formation
     不同演化阶段的分子云与恒星形成的研究
短句来源
更多       
  星的形成
     Barium Star Formation.II.Monte Carlo Analysis
     钡星的形成机制(Ⅱ)Monte Carlo分析
短句来源
     Barium Star Formation Model
     钡星的形成机制模型
短句来源
     Barium Star Formation. (Ⅰ) A Comprehensive Model
     钡星的形成机制(I)完备模型
短句来源
  “star formation”译为未确定词的双语例句
     It is found that the possible exciting star of S141 may be the optical counterpart of the infrared point source 22268+6122, and the lower mass star formation may be taking place in S141.
     电离氢区S141的激发星很可能是位于其边缘的红外点源22268+6122的光学对应体。
短句来源
     Using population synthesis method, the star formation history in globular clusters has been studied.
     本文根据球状星团所特有的金属丰度特征,利用星族综合方法,探讨了球状星团诸恒星的形成史。
短句来源
     The result suggests that the probability of identifying essentially meatal free stars in the local halo is around 6.14×10 -4 —6.14×10 -5 , providing that the star formation in the halo is confined to individual gas clouds with a mass of 10 5 M ? —10 6 M ? .
     如果形成恒星的云的质量为 1 0 6 M - 1 0 7M ,模型结果预言探测到第一代恒星的几率为 6 .1 4× 1 0 - 4 - 6 .1 4× 1 0 - 5 .
短句来源
     The abundances of neutron-capture elements in metal-poor stars, tightly related to the star formation and evolution, provide important clues to the chemical evolution of the Galaxy.
     贫金属星的中子俘获元素丰度与恒星的形成和演化密切相关,它为研究星系形成早期的历史背景和化学演化提供了重要信息。
短句来源
     The star formation history of the elliptical galaxies maybe very complex, but the results can give the observation characters of NGC5018 a good explanation.
     这些结果可以很好地解释NGC5018颜色偏蓝、Mg2谱指数强度偏弱等观测特征.
短句来源
更多       
查询“star formation”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。
  star formation
Based on a CS and C34S survey of dense molecular-cloud cores in regions of high-mass-star formation, we analyze the correlations between line width and size (ΔV-L), as well as between mean density and size (n-L).
      
A ring with active star formation manifests itself on the QBVI map for NGC 834 at a distance of ~15 from its center, and a spiral structure shows up on the QVRI map for NGC 1134 in its inner region.
      
The average spectral energy distribution for these galaxies agrees with the distributions for galaxies with active star formation.
      
The star formation rate in galaxies with zph=5-7 was estimated from their luminosity at λ=1500 ? to be ~30 M⊙yr-1.
      
Statistics of high-velocity outflows in regions of massive star formation
      
更多          


The results of an objective prism survey for H_α emission-line stars in the 5°×5° region around NGC 1333 are presented. We have identified 25 stars as those having the H_α-line in emission, of which 11 had been discovered in the Lick H_α survey. The limiting magnitude of the present survey is about 16.7 mag. in blue. These are suspected to be mainly T Tauri stars. Based on the UGR(Kiso) multiexposure plates, we have found that, on the [(G-U), (R-G)]-diagram, the domain of H_α emission line stars is fairly well...

The results of an objective prism survey for H_α emission-line stars in the 5°×5° region around NGC 1333 are presented. We have identified 25 stars as those having the H_α-line in emission, of which 11 had been discovered in the Lick H_α survey. The limiting magnitude of the present survey is about 16.7 mag. in blue. These are suspected to be mainly T Tauri stars. Based on the UGR(Kiso) multiexposure plates, we have found that, on the [(G-U), (R-G)]-diagram, the domain of H_α emission line stars is fairly well delineated separate from other stars. Some interesting features in their space distribution are also discussed briefly, which may be reflecting the dynamic effects and environmental conditions of star formation.

对恒星形成活跃区NGC1333周围5°×5°区域进行了物端稜镜发射线星巡天观测,此次观测到的H_a发射线星的极限星等约为16.7星等。在此范围內观测到了25颗H_a发射线星(包括11颗已被发现过的L_kH_a星)。这些星在[(G-U),(R-G)]图上的分布与主星序星完全不同。从两色图和暗星云中的空间分布推测,这些发射线星可能大部是金牛座T Tau型星。最后简单讨论了恒星形成区的环境条件。

An equation of state of hot dense matter, whose density and temperature are about 109gcm-3 <ρ3<1015 gcm-3 and 109 K < T < 1011 K, is presented. It is one of the important problems to understand the final stage of star's evolution (e.g. supernova explosion and neutron star formation).In this range of density and temperature, the hot dense matter consists of a mixture of nuclei, neutrons, protons, electrons and neutrinos. When the density is higher than 1012gcm-3, the matter is approximately in beta equilibrium,...

An equation of state of hot dense matter, whose density and temperature are about 109gcm-3 <ρ3<1015 gcm-3 and 109 K < T < 1011 K, is presented. It is one of the important problems to understand the final stage of star's evolution (e.g. supernova explosion and neutron star formation).In this range of density and temperature, the hot dense matter consists of a mixture of nuclei, neutrons, protons, electrons and neutrinos. When the density is higher than 1012gcm-3, the matter is approximately in beta equilibrium, and when the density is lower, it is in the nuclear statistical equilibrium. We consider nuclei as Boltzman particles in the ground state and neglect the effects associated with their finite size and excited states. By minimization of free energy for A and Z, one can choose a nuclear species to represent the mean effects of heavy nuclei and take alpha particles to represent the mean effects of light nuclei. The electrons and neutrinos can be treated as ideal Fermions. We use Waleck's relativistie mean field approch (RMFA) to describe the neutrons and protons. The compositions of the matter can be determined by equilibrium conditions. Because RMFA is Lorentz-covariant and includes explicitly meson degrees of freedom, the results of the equation may be more responsible in high-density region.In table 1, a comparison between the results of reference [1] and ours is given. It shows that they are in good agreement, so we conclude that the lower-density part of the equation does not depend on physical model strongly. Fig. 1 gives a comparison of the nuclear species in the hot dense matter between reference [10] and ours. There are upper limits for A and Z in curves of reference [10], but there are none in ours. It seems to be more appropriate to determine the nuclear species by minimization of free energy at certain conditions. In higher-density region, our equation is stiffer than the equation in reference [3] (see Fig. 2), and the maximum adiabatic index is about 4 (see table 2). Because the pressures of neutron and proton dominate the total pressure in this region, the equation may affect the results of simulation calculation of stellar core collapse, and this may be an important problem to study the final stage of star's evolution. Our equation does not conflict with the 'causality' condition (see Pig. 3).

本文提出了一个温度和密度分别在:10~9K T 10~(11)K;10~9gcm~(-3) ρ 10~(15)gcm~(-3)范围的热密物质状态方程.主要考虑了核子的相对论效应和确定原子核种类的方法.所得结果表明核子的相对论效应使状态方程高密部分明显地硬化(核子比熵为1k_B的等熵线最大绝热指数约为4);采用自由能取极小值的方法确定原子核的种类比较合理.

The general perspective and the recent advances of the density wave theory of spiral galaxies are summarized and reviewed.As Oort pointed out in 1962, the major problem in this field is how to explain the existence and the maintenance of the large-scale regular spiral patterns in a system of strongly differential rotation and the prominence of the two-armed features. The main purpose of the modal theory of density wave, which has been successfully developed by Lin and has collaborators during the last two decades,...

The general perspective and the recent advances of the density wave theory of spiral galaxies are summarized and reviewed.As Oort pointed out in 1962, the major problem in this field is how to explain the existence and the maintenance of the large-scale regular spiral patterns in a system of strongly differential rotation and the prominence of the two-armed features. The main purpose of the modal theory of density wave, which has been successfully developed by Lin and has collaborators during the last two decades, is simply to explain the large-scale regular structure, the "grand design", rather than the local, detailed and less regulat features.Since the morphological classification of galaxies is based on the large-scale regular structure, the modal theory is appropriate for the investigation of the dynamical basis of the morphological classification. The coexistence of large-scale regular structure and relatively irregular features suggests that the modal approach and the initial value approach are complementary rather than contradictory.The overall picture of the structure of the theory can be sketched as in Fig.1. Two types of over-reflection of waves near the corotation are briefly described. The modes consisting of long and short trailing waves were first established by Lin and Lau and later extended to more general situations by Lin's collaborators. A sizable bulge in the center or the "Q-barrier" plays an important role in maintaining the normal spirals, and the inner Lindblad resonance holds the key to the prominence of the two-armed features.In addition to the long and short waves, the third category of waves, the open waves, has been found recently by using the Lau-Bertin cubic dispersion relationship (see Lin and Berlin[10]). It was found that the (J, Q) plane could be divided into two regions where over-reflections of Type I and II are important respectively.The most important application of the density wave theory in the 1960's was to give explanations to a lot of astronomical observations and the mechanism for the star formation in terms of the dispersion relationship and the galactic shock wave, while the most important application of the theory during the second stage, roughly since early 1970's, is the dynamical classification of galaxies in terms of the investigation of modes. Convincing results along this line have been obtained by Lin and his collaborators during the last years. By changing the functions of the basic state σ0,(r), Ω(r) and Q(r) systematically, they obtained the transition from tightly wound to open spiral modes and the transition from normal t?barred spiral modes as shown in Fig.5 and Fig.6 respectively.Although the modal approach is different from the initial value approach, some kind of evolution can be investigated by superposition of modes with different pattern velocities and different growth rates.

本文对密度波理论的总的观点和近年来取得的新进展作了概括和评述。

 
<< 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star formation的内容
在知识搜索中查有关star formation的内容
在数字搜索中查有关star formation的内容
在概念知识元中查有关star formation的内容
在学术趋势中查有关star formation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