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gamma
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    The Performance and Development of Lunar Gamma Ray Spectrometer
    月球玛射线谱仪的研制及其性能
短句来源
    The resonant inverse Compton scattering (RICS) of the relativistic electrons in an intense magnetic field is an efficient radiation mechanism to produce the high energy gamma rays.
    强磁场中的共振逆康普顿散射(RICS)是产生玛射线的有效机制.
短句来源
  伽玛
    The Performance and Development of Lunar Gamma Ray Spectrometer
    月球伽玛射线谱仪的研制及其性能
短句来源
    The resonant inverse Compton scattering (RICS) of the relativistic electrons in an intense magnetic field is an efficient radiation mechanism to produce the high energy gamma rays.
    强磁场中的共振逆康普顿散射(RICS)是产生伽玛射线的有效机制.
短句来源
  “gamma”译为未确定词的双语例句
    Timing Analysis of the Gamma ray Pulsar Geminga with a Phase Cross correlation Method
    用位相相关方法测量Geminga脉冲星的守时参数
短句来源
    Blazar is mainly characterized by rapid variability with a large amplitude, high polarization, compact radio radiation, and nonthermal radiation in the electromagnetic wave from radio bands to gamma rays. An important research aspect for the blazar is the unification and evolution of blazar.
    大幅度快速光变、高偏振、整个电磁波段的非热连续辐射及致密的射电辐射是blazar天体的主要特征,blazar天体的统一与演化是blazar天体研究的重要内容。
短句来源
    On the basis of the model that a neutron star accretes the comet clouds around it, we put forward that the soft gamma ray repeater GB790107 originates from the weak magnetic field (~108G) old neutron star.
    本文在中子星吸积彗星云模型的基础上,认为软重爆GB790107起源于弱磁化(B~10~8G)中子星,其阵雨式地吸积彗星云将在中子星表面形成一光厚辐射区,该辐射区的温度分布由激波模型确定.
短句来源
    By direct detection the experiments look for the signal when the dark matter particles scatter off the nuclei of the detector material; by indirect detection the experiments look for the annihilation products of dark matter, such as the high energy gamma rays, neutrinos, positrons or anti-protons.
    直接探测实验探测的是暗物质粒子与探测器物质碰撞所留下的信号,而间接探测实验则寻找暗物质湮灭的产物,如高能伽马射线、高能中微子、正电子和反质子等。
短句来源
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  gamma
It is also shown that on the nilmanifold $\Gamma\backslash (H^3\times H^3)$ the balanced condition is not stable under small deformations.
      
For $\gamma\in\mathbb{R}$ let $C(\gamma)$ be the set of all $f\in{\mathcal S}^\prime$ for which$\sum_{n=0}^{\infty}\,|(f,h_n)|\,(n+1)^{\gamma}>amp;lt;\infty$, where $(h_n)_{n=0,1,\dots}$ is the orthonormal base of Hermite functions.
      
We show that $C(\gamma)\subset S_0$ if and only if $\gamma\geq\frac{1}{4}$ and that $S_0\subset C(\gamma)$ if and only if $\gamma\leq{-}\frac{1}{4}$.
      
Using these results we give an explicit solution of the problem of optimal reconstruction of functions from Sobolev's classes $W^{\gamma}_{p}(M^{d})$ in $L_{q}(M^{d}), 1 \leq q \leq p \leq \infty$.
      
This result generalizes the characterization of Fourier series of distributions with a distributional point value given in [5] by $\lim_{x\rightarrow\infty}\sum_{-x\leq n\leq ax}a_{n}e^{inx_{0}}=\gamma\ (\mathrm{C},k)\,$.
      
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In this paper, we propose a model to explain the energy supply of cosmic γ-ray burst by means of magnetic energy annihilation in neutral sheets formed in local active region on the magnetic white dwarf. According to this model the instability process in plasma consists of two phases, namely, the thermal explosive phase and the steady annihilation phase. The magnetic energy stored in the local source is efficiently converted into kinetic energy and cosmic dissipation energy of plasma at a rate that is consistent...

In this paper, we propose a model to explain the energy supply of cosmic γ-ray burst by means of magnetic energy annihilation in neutral sheets formed in local active region on the magnetic white dwarf. According to this model the instability process in plasma consists of two phases, namely, the thermal explosive phase and the steady annihilation phase. The magnetic energy stored in the local source is efficiently converted into kinetic energy and cosmic dissipation energy of plasma at a rate that is consistent with the observations. With the rapid increasing of anomalous resistivity a plasma turbulence field is set up which can immediately be coupled with fast electrons in the Maxwellian high energy tail. Then the relativistic electrons are produced within a time as short as 10~-8 sec. which is not conflicting with the fast ascent of brief“spike”of gamma rays. The results of calculation indicate also that the γ-rays can be emitted by the accelerated electrons moving around the magnetic field through Synchrotron radiation. Of course, many details of this theoretical model still remain to be cleared up. However some points of view which have been discussed here may be taken as a basis for future work.

本文对宇宙r射线暴的能源提出了一个模型。按照这种模型,等离子体的不稳定过程包含两个相,即热暴发相和稳定湮灭相。而贮存在局部源中的磁能,以一种与观测相一致的速率有效地转换为等离子体的动力能和欧姆耗散能。随着反常阻抗的快速增加,建立了等离子体的湍动场。它与麦克思韦高能尾巴电子迅速耦合,产生了相对论性电子。r射线能够通过相对论性电子在磁场中的同步辐射而得到说明。

The modified gamma-distribution function of dust particles, f(γ), which can be determined from tail brightness profiles on the basis of mechanical theory, is discussed with special regard to its reliability and accuracy. Physical significance of f(γ) is also discussed in terms of dust model parameters, and it is shown that f(γ), if treated carefully, will serve as an effective tool in studying cometary dust. Four isophotes of Comet Arend-Roland, 1957 Ⅲ, in the orange-red light (λλ0.53—0.68 micron) obtained...

The modified gamma-distribution function of dust particles, f(γ), which can be determined from tail brightness profiles on the basis of mechanical theory, is discussed with special regard to its reliability and accuracy. Physical significance of f(γ) is also discussed in terms of dust model parameters, and it is shown that f(γ), if treated carefully, will serve as an effective tool in studying cometary dust. Four isophotes of Comet Arend-Roland, 1957 Ⅲ, in the orange-red light (λλ0.53—0.68 micron) obtained by Ceplecha (1958), are analysed by the numerical method described in Paper Ⅰ (Kimura and Liu 1975) with some improvements and higher approximations. The distribution f(γ) thus obtained shows a bimodal character peaked at γ=0.10 and 0.010 with a height ratio of 1 to 0.6. Dust emission rate, which is assumed to follow the inverse square law of heliocentric distance, is estimated to give P_dC_(sca)=(1.3±0.5)×10~9 cm~2/sec, where P_d is the rate of particle emission at 1 a.u. and C_(sca) is a mean effective cross section of particles for light scattering including phase effect (the scattering angles of present interest range from about 80 to 100 degrees).

本文讨论了,分析彗尾亮度而求出的“修正的γ-分布函数”f(γ)的意义,f(γ)与尘埃模型的物理量的关系,以及f(γ)做为检验尘埃模型的手段的有效性。根据文[1]所提方法,详细考虑了该方法中存在的各种因数,求出高精度的“修正的γ-分布函数”f(γ)。对Arend-Roland彗星求得的f(γ)函数是γ=0.10和0.01,相对高度为1:0.6的双峰分布。假设粒子抛射率反比于彗核太阳距离的平方,一天文单位时的粒子抛射率P_d,将是P_d

Cosmic Gamma-ray Bursts are a sort of astrophysical phenomena which can release extremely high energy. Recently, more than hundred bursts have been detected since it was discovered in 1973. Time structure, spectrum and intensity of many bursts have been published and position of a few bursi sources have also been reported. This paper describes some statistical characteristics of Cosmic Gamma-ray Burst.

宇宙γ射线爆发是一种极高能量的天体物理现象。现已探测到100多个爆发事件,得到了它们的时间结构、能谱、强度和部分辐射源的位置。本文将逐个介绍宇宙γ射线爆发的统计结果。

 
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