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stellar     
相关语句
  恒星
    THE STELLAR "FLARE" MODEL FOR COSMIC γ-RAY BURST
    宇宙γ射线爆的恒星“耀斑”模型
短句来源
    STELLAR“SUPERFLARE”MODEL FOR COSMIC γ-RAY BURST
    宇宙γ射线爆的恒星“超耀斑”模型
短句来源
    THE PHASE SHIFTS BETWEEN STELLAR ARM AND GASEONS ARM IN SPIRAL GALAXIES M81 AND M51
    旋涡星系M81,M51的恒星臂与气体臂的相移
短句来源
    STABILITY OF STELLAR STRUCTURE IN NON-EQUILIBRIUM THERMODYNAMICS (Ⅰ)——PP Ⅰ REACTION
    非平衡热力学中恒星结构的稳定性研究(Ⅰ)——PPⅠ反应
短句来源
    THE CONSISTENT SOLUTION FOR BOTH THE GALACTIC GASEOUS SHOCK AND LINEAR STELLAR DENSITY WAVE
    星际气体激波与恒星线性密度波的总合自洽解
短句来源
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  星的
    (U-B)_T~o ranges from 0.43 for E galaxies to-0.33 for I_m galaxies. 541 galaxie formed an obvious sequence along a diagonal of the two color diagram (B-V)_T~o-(U-B)_T~o. This can be explaned by the different mixture of stellar population,which made up the galaxies.
    (U-B)_T~O从E系的0.43到I_m系的-0.33.541个星系在(B-V)_T~O-(U-B)_T~O两色图上沿一条对角线形成一个明显的序列,这可以从组成星系的红兰星的混合效应得到解释。
短句来源
    541 galaxie formed an obvious sequence along a diagonal of the two color diagram (B-V)_T~o (U-B)_T~o. This can be explaned by the different mixture of stellar population, which made up the galaxies.
    541个星系在(B-V)_T~O-(U-B)_T~O两色图上沿一条对角线形成一个明显的序列,这可以从组成星系的红兰星的混合效应得到解释。
短句来源
    In this paper, we use Kurucz stellar atmosphere model and black-body model to fit for the observational data in ultraviolet, optical, near-IR and IRAS bands for the 22 Herbig Ae/Be stars, and use the method of energy balance to analyze the ratio of the energy dissipation of the central stars and the energy reradiation from the dust shells statistically, we conclude that the morphological type of the circu-mstellar dust shell of Herbig Ae/Be star is disk-shaped.
    我们使用Kurucz恒星大气模型以及黑体模型对22颗Herbig Ae/Be星的紫外数据、IRAS观测数据、地面光学及近红外测光数据资料等进行了拟合计算,用能量平衡方法进行了统计分析,得出Herbig Ae/Be星的尘埃壳层为盘状的结论.
短句来源
    From the distribution of rotation period and convection parameter of M type stars, stellar chromospheric activity of M type stars depart from the anticipation of a.
    A—早F型主序恒星的自转周期和恒星对流区的随色指数的分布明显地影响着这些恒星的色球活动行为。 而M型主序星的色球活动水平基本上随自转参量的增大呈上升趋势,并且M型主序星的色球活动水平在色指数较大时趋于饱和。
短句来源
    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。
短句来源
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  星体的
    Infrared Observations and Studies of Young Stellar Objects
    年轻星体的近红外观测与研究
短句来源
    A Study of the Spectral Energy Distribution of Massive Young Stellar Objects in the Infrared
    大质量年轻星体的红外谱研究
短句来源
    ~13CO(1→0) LINE EMISSION FROM MASSIVE YONG STELLAR OBJECTS
    大质量年轻星体的~(13)CO(1→0)谱线发射
短句来源
  星体
    ABNORMAL NEUTRON STAR WITH ABNORMAL PROTONS II. INHOMOGENEOUS STELLAR MODEL
    含有反常质子的反常中子星II.非均匀星体模型
短句来源
    Infrared Observations and Studies of Young Stellar Objects
    年轻星体的近红外观测与研究
短句来源
    A Study of the Spectral Energy Distribution of Massive Young Stellar Objects in the Infrared
    大质量年轻星体的红外谱研究
短句来源
    ~13CO(1→0) LINE EMISSION FROM MASSIVE YONG STELLAR OBJECTS
    大质量年轻星体的~(13)CO(1→0)谱线发射
短句来源
    Order of Magnitude in the Calculation of the Stellar Structure
    星体结构计算中的数量级估计
短句来源
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  stellar
The infrared spectrometer operates in the range of 1-1.7 μm with a resolution of 3.5 cm-1 in the mode of nadir observations and solar and stellar occulations.
      
Large-scale movements in convective stellar envelopes are studied by the methods of hydrodynamics, taking account of the compressibility of the gas, rotation, gravitation, and anisotropic turbulent viscosity.
      
Specific calculations are carried out for typical values of the near-stellar gas parameters.
      
Calculation of flow of stellar wind past an x-ray source
      
In the cited works [1, 2], a study was made of supersonic flow round a source of x-ray radiation by stellar wind.
      
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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...

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.

It has been shown by S. A. Zhevakin that the critical double ionizarion zone of helium Hell in the envelope of a pulsating star, such as RR Lyrae, is a mechanism giving rise to the auto-oscillation of the star. The mass of the star should have such a value that its Hell zone has a definite non-adiabatic degree of oscillation, so as to excite its auto-oscillation. In the present paper the mass of RR Lyrae is determined on the basis of Zhevakin's theory of stellar variability.The mass of RR Lyrae is first...

It has been shown by S. A. Zhevakin that the critical double ionizarion zone of helium Hell in the envelope of a pulsating star, such as RR Lyrae, is a mechanism giving rise to the auto-oscillation of the star. The mass of the star should have such a value that its Hell zone has a definite non-adiabatic degree of oscillation, so as to excite its auto-oscillation. In the present paper the mass of RR Lyrae is determined on the basis of Zhevakin's theory of stellar variability.The mass of RR Lyrae is first assumed to have Sandage's value 1.15 M⊙. Accurate calculations of various physical quantities in the envelope of RR Lyrae are made. The non-adiabatic degree of oscillation in the Hell zone is found to be y = 3.16, which is not admissible by Zhevakin's theory of stellar variability, so that the mass M of RR Lyrae cannot be 1.15M⊙.In order to estimate the mass of RR Lyrae, we use a relation between y and M, given by Zhevakin, based on the supposition that the stellar envelope is built on polytrope of index n. It is found for RR Lyrae that the polytropic index n is 2.818, so that the mass M lies between 0.47 M⊙ and 0.99 M⊙. On the other hand Oke and Bonsack concluded from the spectrum analysis of RR Lyrae and the period-density relation, that the mass M of RR Lyrae is substantially less than the solar mass M⊙. Based upon all these considerations we choose a possible value of M to be 0.85 M⊙ and make all the calculations anew. We find that y = 2.27 for M = 0.85 M⊙, which satisfies Zhevakin's condition (7.1). We hope that further observations will decide whether the mass M of RR Lyrae is really equal to 0.85 M⊙.

这是根据日瓦金的造父变星理论来间接确定造父变星质量的一个新方法.现用这方法求天琴座RR星的质量.按照这个理论,变星的质量必须对应于它的振动非绝热度.计算指出,桑德吉的结论,天琴座RR星的质量为1.15M不能成立.从日瓦金星体包层是多层球的近似理论及光谱分析方面的考虑,我们假定天琴座RR星的质量为0.85M.从这个数值计算出的振动非绝热度同日瓦金理论中对造父变星的条件相符合.这证明0.85M的值是该变星质量的可能值.至于这是否真正代表该星的质量,尚待进一步天文观测的证实.

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...

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.

 
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