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
   luminosity 在 天文学 分类中 的翻译结果: 查询用时:0.171秒
图标索引 在分类学科中查询
所有学科
天文学
物理学
核科学技术
环境科学与资源利用
自动化技术
生物学
燃料化工
石油天然气工业
林业
更多类别查询

图标索引 历史查询
 

luminosity
相关语句
  光度
    Radio Observational Studies of High Luminosity AGNs and the Dim Galactic Center Object Sgr A~*
    高光度活动星系核和暗弱银心天体Sgr A~*的射电观测研究
短句来源
    STATISTICAL ANALYSES OF RADIO LUMINOSITY OF PULSARS
    脉冲星射电光度的统计分析
短句来源
    THE LUMINOSITY FUNCTION AND H-R DIAGRAM
    白矮星的光度函数与H—R图
短句来源
    The Nuclear Luminosity and Mass of Type I Seyfert Galaxies
    Ⅰ型塞佛特星系核的光度和质量
短句来源
    The Spatial Density Distribution and Luminosity Function of OH/IR Maser Sources
    OH/IR脉泽源的空间分布和光度函数
短句来源
更多       
  亮度
    The early type galaxies with luminosity Mr-20.5 show the brightest surface brightness.
    暗红星系的大小分布具有不依赖于自身光度的特征。 M_r~20.5的早型星系具有最高的表面亮度
短句来源
    The model with substructures can suppress the luminous central galaxy formation in cluster and can give a better luminosity function compared with the observation.
    考虑到次结构一方面可以降低中心星系的亮度,同时能预言与观测很接近的光度函数形状。
短句来源
    A luminosity function is the number of objects of a particular sort as a function of their luminosity or brightness in some wavelength band.
    光度函数是作为某一波段的光度或亮度的函数的特定种类的天体数目。
短句来源
  “luminosity”译为未确定词的双语例句
    The Properties of the Variation in Luminosity of NGC4051
    Seyfert星系NGC4051的光变特性
短句来源
    The resulting q_0-values from 8 largely independent samples of radio quasars all fall within the 4σ range obtained in [1], namely, 1.0≤q_0≤3.5. The most important assumption made is that the characteristic luminosity of radio quasars is independent of the cosmic epoch.
    从8个射电类星体的样品子集计算所得的q_0值,全部落在1.0≤q_0≤3.5范围内.
短句来源
    The range of luminosity of identified OH/IR sources is approximately from 0.16 Jy· kpc2 to 1000 Jy kpc2. It is quite different from that of unidentified OH sources.
    由文中结果得到银河系中有光学或红外对应体的OH/IR脉泽源约2×10~5个,大部分未探测到的OH/IR源,其流量密度可能在0.1—1Jy之间.
短句来源
    We present here an observational result for the hard X-ray spectrum of Cyg X-1 in 20-200 keV range, which was obtained by a balloon-borne CsI-NaI phoswich type telescope launched at Xianhe Balloon Facilities on Sep. 22, 1985. The X-ray luminosity in 10-200 keV is estimated as (1.07 ± 0.08) × 1037 ergs/s.
    1985年9月22日,我们用空间硬X射线望远镜HAPI-2,在我国的高空气球上,对天鹅座X-1进行了观测,望远镜几何面积为140cm~2,观测能区20—200keV,空间定向精度±0.2°。 获得的硬X射线能谱陡,总辐射能流LX~1.0×1~(37)erg/sec,低于常规态。
短句来源
    An IRAS galaxy sample with infrared luminosity high up to 10 11.8 to 10 12.8 L ⊙ was observed using the Australia Compact Array (ATCA) at 8.6, 4.8, 2.4 and 1.4 GHz.
    使用澳大利亚致密阵 (ATCA)对一个红外光度高达 1 0 1 1 .8- 1 0 1 2 .8L⊙ 的IRAS星系样本进行了 8.6 ,4.8,2 .4和 1 .4GHz的射电观测 .
短句来源
更多       
查询“luminosity”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。
  luminosity
For each observational period, the time dependence of the atmospheric luminosity and absorption is obtained.
      
Serial panoramic monochromatic maps of the intensity of luminosity of the upper atmosphere emissions measured from orbiting detectors can serve as a main data source for such an analysis.
      
Results are given of the investigation of self-luminosity of flow in hypersonic wind tunnels with electric-arc heaters, and the possibilities of using this luminosity for the visualization of flow past bodies are analyzed.
      
It is demonstrated that the luminosity is caused by nonequilibrium physicochemical processes in nozzles and is defined by the excitation of low-potential electron-vibrational levels of molecules and atoms of impurities in the flow.
      
It follows from comparison of flow patterns obtained by the shadow method with photographs of flow in the vicinity of bodies that the use of luminosity for determining the structure of flow past models is not always justified.
      
更多          


Ⅱ.The Various Results of the Correction to the Zero Point of the P-L Relation and of the Absolute Magnitude of the RR Lyrae Variables 31 results including 3 results of this paper in connection with the zero point of the period- luminosity relation since Wilson's result of 1939 are tabulated.They are collected in 6 tables according both to the nature of the results and the methods used.A comment for each result is made. Table 1 The Difference,Δ'M_(pg),between the Observed and the Computed Magnitudes (O-C)...

Ⅱ.The Various Results of the Correction to the Zero Point of the P-L Relation and of the Absolute Magnitude of the RR Lyrae Variables 31 results including 3 results of this paper in connection with the zero point of the period- luminosity relation since Wilson's result of 1939 are tabulated.They are collected in 6 tables according both to the nature of the results and the methods used.A comment for each result is made. Table 1 The Difference,Δ'M_(pg),between the Observed and the Computed Magnitudes (O-C) (The computed magnitudes are based on Shapley's P-L relation and the absolute magnitude of the RR Lyrae variables,=00).

在第一节引言里,说明了造父变星周光关系在天文学上的重要性;叙述了沙泊莱周光关系以及周光关系零点问题发生疑难的经过和对待这问题本题作者的看法.第二节里胪列了自1939年以来关于造父变星零点的31个结果,包括本文的3个结果.按照结果的性质和所用的方法分6表列出.对每个结果进行了扼要的说明或讨论,对其中不能采用的11个结果有较详的评论.沙泊莱周光关系的另点暗了1星等多是根据威尔逊的结果,后者所以有这项大的差异,在本文里完全得到解释.第三节里推导出了同时对星的视星等和绝对星等瀰散的改正式和对于造父变星的应用法,也给出了平均距离和平均视差之积,的正确公式.最后,在第四节里,把所有可用的结果总起来求出3个权重平均值;1个是差值,即观测星等和根据周光关系以及天琴座 RR 型星绝对星等所算得的星等,两者的差,1个是周光关系零点改正值;最后1个是天琴座 RR 型星的绝对星等值.把这3项结果统一考虑,对第1项结果给以2倍的权重,最后得到对沙泊莱周光关系的零点政正是-1~m.28,天琴座 RR 型星的绝对星等是+0~m.34.

In the first introductory part it is pointed out that the main difference among current theories of stellar evolution is in the evolutionary stage after stars move onto the main sequence.Three kinds of theory are mentioned.The first is the theory of stellar evolution with constant mass,the second is the corpuscular emission theory of stellar evolution,and the third is the theory of direct evolution of main sequence stars to white dwarfs.The second part introduces the first theory.The difficulty of this theory,as...

In the first introductory part it is pointed out that the main difference among current theories of stellar evolution is in the evolutionary stage after stars move onto the main sequence.Three kinds of theory are mentioned.The first is the theory of stellar evolution with constant mass,the second is the corpuscular emission theory of stellar evolution,and the third is the theory of direct evolution of main sequence stars to white dwarfs.The second part introduces the first theory.The difficulty of this theory,as is well known,is how to effect the evolution to white dwarfs of the main sequence stars after they have evolved to red giants and/or supergiants.Observational evidence is scanty,and,above all,theoretically,it is blank. In the third part,the second theory is stated.This theory,as we point out,should contain the following assumption:either it denies the existence of the initial luminosity function of main sequence stars,or it requires the relation 0 (μ_0) between the initial mass of a star0,and its initial mean molecular weight,μ_0,exactly the same as the relation(μ) between the mass of the staand its mean molecular weight,μ, after the evolution by corpuscular emission.Neither of these two is likely possible. Moreover,the essential data,derived from investigation of stellar structure,on which this theory is based is not reliable as compared to the current ones,obtained by much more careful considerations in the same field of investigation.Hence this theory is not trustworthy. The fourth part relates about the third theory.It is pointed out that the key point of this theory is whether a main sequence star will evolve with its chemical composition homogeneous throughout the whole star and thus shift to the left of the main sequence so as finally to be able to evolve to a white dwarf.

在第一部分引言中,说明现代恒星演化学说的分歧主要是在恒星形成主序星以后的演化.本文叙述三种学说:第一种是质量固定的恒星演化学说,第二种是微粒发射的恒星演化学说,第三种是主序星径向白矮星的演化学说.第二部分介绍第一种学说,指出困难之点在恒星脱离主星序演变成红巨星、超巨星后,怎样演化到白矮星的问题,观测资料既贫乏,理论方面更是空白.第三部分介绍第二种学说,指出这学说蕴含着下面的假定:或是否认主序星原始光度函数的存在,或是要求主序星的原始质量 m_0和原始平均分子量μ_0的关系 m_0(μ_0)恰好是因微粒发射后所演变成的质量 m 和平均分子量μ的关系 m(μ).这两者都是很少可能的.而这学说所根据从内部结构理论得到的主要数据,就近几年来好些同类研究,用较精密方法所得的计算结果来说,显然是不正确的.所以这学说的可靠性是很小的.第四部分介绍第三种学说,指出这学说的主要关键在一般的主序星能否因自转而使恒星的化学成份保持为内外均匀的星型,从而在赫-罗图上自主序星向左演变,演化为白矮星.

The emission mechanism from X-ray soturces in close binary stars is studied.It is suggested that pair production may play an important role in the X-ray emission region which is formed by the accretion of a compact object(a neutron star or a black hole).The present model accounts qualitatively for the following observed general properties in X-ray binaries: 1.The X-ray luminosity lies within the range 10~(36)—10~(38)erg/sec. 2.The X-ray energy spectrum can in the majority of cases be represented either...

The emission mechanism from X-ray soturces in close binary stars is studied.It is suggested that pair production may play an important role in the X-ray emission region which is formed by the accretion of a compact object(a neutron star or a black hole).The present model accounts qualitatively for the following observed general properties in X-ray binaries: 1.The X-ray luminosity lies within the range 10~(36)—10~(38)erg/sec. 2.The X-ray energy spectrum can in the majority of cases be represented either the power-law or the thermal bremsstrahlung form. 3.The temperature of the thermal bremsstrahlung spectrum is the order of 10~8K. 4.The form of the energy spectrum does not change appreciably when the luminosity fluctuates.

本文研究了密近双星中的 X 射线源的发射机制.本文提出:在致密星(中子星或黑洞)的吸积所形成的 X 射线发射区中,电子对的产生起着重要的作用.这种模型可以定性地说明 X射线双星所具有的几个一般的观测特征,即:1.它们的 X 射线光度都在10~(36)—10~(38)尔格/秒范围中.2.X 射线能谱为幂形式,或热韧致形式.3.热韧致谱的温度数量级为10~K.4.当光度涨落时,能谱形式无明显变化.

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