perigalactic distance meaning in Chinese
近银心距
Examples
- The differences in orbital morphologies due to different potentials is slighting , however , given a certain potential , for clusters that have perigalactic distance smaller than 1 kpc , some orbits may exhibit a chaotic behavior . the correlation between the metallicity of samples and the orbital morphologies is unclearly ; ( 4 ) it is found that the semi - major axis , apogalactic distance and azimuth period of 29 sample clusters are changed with their metallicity similarly , but a obvious correlation is seen between orbital eccentricity and metallicity . there is a fraction of 24 % of the sample clusters with eccentricities lower than 0 . 4
不同的引力势模型对球状星团轨道的具体形态影响不大，在给定的引力势模型下，当某些星团的运动轨道穿越距银心1kpc附近的区域时会出现“混沌”现象： ( 4 ) 29个样本星团的轨道半长轴、远银心距和方位周期随金属度的变化规律基本相似，样本星团的金属度与其轨道形态之间的相关性并不明显，然而轨道偏心率与金属度有关，对于所选的晕族样本星团而言，大约有24的样本星团的轨道偏心率低于0 . 4 。 - The different galactic gravitational potential have not clear influence upon the perigalactic distance , eccentricity and uncertainty of orbital parameters , but which is significant for other parameters , such as the apogalactic distance , semi - major axis , radial period and azimuth period and so on ; ( 5 ) the monte carlo simulation show that : the distribution morphologies of the orbital parameters which are produced by simulation data are separated into three types : gaussian profile , semi - gaussian profile and non - gaussian profile
不同的引力势模型对近银心距、偏心率和参数的不确定度等量影响较小，但是对远银心距、轨道半长轴、径向周期和方位周期等参数影响较为明显。 ( 5 ) montecarlo模拟的结果表明：根据模拟观测数据得到的轨道参数的分布形态大致可分为三类：高斯分布、准高斯分布和非高斯分布；观测数据对轨道参数的影响与样本的选取、轨道参数的类型等有关。