空间密度分布的英文

• spatial density distribution

• "空间"英文翻译    space; enclosure; room; blan ...
• "密度"英文翻译    density; thickness
• "分布"英文翻译    distribute; spread; scatter; ...
• "空间密度" 英文翻译 :    space density; spatial density
• "相空间密度" 英文翻译 :    phase space density
• "空间密度轮廓" 英文翻译 :    ace de ity profile; space density profile
• "密度分布" 英文翻译 :    density distribution; density portion
• "密度分布图" 英文翻译 :    density profile
• "源密度分布" 英文翻译 :    source density distribution
• "电流密度分布" 英文翻译 :    current density destribution; current density distribution
• "电子密度分布" 英文翻译 :    electron density distribution; electron-density distribution
• "方位密度分布" 英文翻译 :    orientation density distribution
• "概率密度分布" 英文翻译 :    probability density distribution
• "功率密度分布" 英文翻译 :    power density distribution; power-density distribution
• "裂变密度分布" 英文翻译 :    fission distribution
• "密度分布函数" 英文翻译 :    density function
• "密度分布梯度" 英文翻译 :    density distribution gradient
• "能量密度分布" 英文翻译 :    energy density distribution
• "偶极密度分布" 英文翻译 :    double density distribution
• "缺陷密度分布" 英文翻译 :    defect density distribution
• "失效密度分布" 英文翻译 :    failure-density distribution
• "振幅密度分布" 英文翻译 :    amplitude density distribution
• "中子密度分布" 英文翻译 :    neutron density distribution; neutron densuty distribution
• "空间强度分布" 英文翻译 :    spatial intensity distribution
• "等离子密度分布" 英文翻译 :    plasma density profile

• Comparing with the current observations , which include the number density distribution in space , mass function , etc . , the so - called standard modes for both the power law and gaussian cluster initial mass functions are selected among many runs of simulations . the deviation from the standard modes , which is resulted from the change of the parameter for the initial conditions , is discussed in detail . the discussion of the model parameters is also presented although they are adopted as the typical values based on previous work
  对应一定的初始分布我们发现无论是幂律的还是对数高斯的球状星团初始质量谱经过长时间的动力学演化都会得到和现在银河系观测到的球状星团系统相符的对数高斯的质量分布；动力学演化会明显地改变球状星团系统的空间密度分布，靠近银心区域的球状星团瓦解得更多；经过动力学演化后的球状星团速度分布函数在靠近银心的区域明显得不同于初始分布，初始拥有较大轨道偏心率的球状星团更容易瓦解。
• Given the initial conditions including ( 1 ) number density distribution in space which has the similar form to the present day ones , ( 2 ) both the power law and gaussian mass functions for clusters , and ( 3 ) two different velocity distributions which one has a constant dispersion and the other is described by the eddington formula , the dynamical evolution of globular clusters in our milky way galaxy is investigated in detail by means of monte carlo simulations
  本文采用与观测结果具有相同形式的球状星团空间密度分布函数，在给定两种球状星团系统的初始质量谱(幂律的和对数高斯的)和两种球状星团系统的初始速度分布函数(爱丁顿速度分布函数和常数的速度弥散度)条件下，我们采用montecarlo的方法对球状星团系统的动力学演化进行讨论。