半长轴的英文

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"半长轴"怎么读用"半长轴"造句

英文翻译手机版

major semi-axis
semimajor axis

"半"英文翻译 half
"长轴"英文翻译 major axis; long axis; macro ...
"axis半长轴" 英文翻译 : semimajor
"半长轴坡面" 英文翻译 : hemi-macro dome
"轨道半长轴" 英文翻译 : semi-major axis of ellipse
"长轴" 英文翻译 : [数学] major axis; long axis; macro axis; prolate axis
"半长径" 英文翻译 : semi-major axis
"半长卡" 英文翻译 : card, half-size; half-size card; halfsize cardd
"半长裤" 英文翻译 : clamdiggers
"半长裙" 英文翻译 : long half slip
"半长同" 英文翻译 : semi major axis
"半长靴" 英文翻译 : bottine
"长轴端" 英文翻译 : apsis
"长轴观" 英文翻译 : long-axis view
"长轴类" 英文翻译 : long-axones
"长轴面" 英文翻译 : macropinacoid
"长轴位" 英文翻译 : long axis view; long-axis
"长轴柱" 英文翻译 : macroprism
"长轴锥" 英文翻译 : macropyramid
"伸长轴" 英文翻译 : axis of elongation
"生长轴" 英文翻译 : growth axis
"牙长轴" 英文翻译 : long axis of tooth
"延长轴" 英文翻译 : spindle extension
"纵长轴" 英文翻译 : fore and aft axis
"半长度错觉" 英文翻译 : half length illusion; halflength illusionn; length illusion

例句与用法

Either half of the major axis is called a semimajor axis .
长轴的每一半叫做半长轴。
The major semiaxis a and p of the relative orbital motion are known .
我们知道其相对轨道运动的主要半长轴a和周期p。
The major semiaxis a and p of the relative orbital motion are known
我们知道其相对轨道运动的主要半长轴a和周期p 。
Based on the first order perturbing solutions , the thesis obtained the long term relative perturbation of equal semi - major axis formation , which is removed by adjusting semi - major axis of the flying - around satellite
接着，基于一阶摄动解，得出了等半长轴绕飞编队的长期相对摄动规律，并通过调整环绕卫星的半长轴消除了长期相对摄动。
Based on the first order perturbing solutions due to the earth oblateness , the long term relative perturbation of equal semi - major axis formation is analyzed , which is removed by adjusting semi - major axis of the flying - around satellite
在地球扁率摄动一阶解的基础上，分析了等半长轴编队飞行的长期相对摄动规律，并提出了消除长期相对摄动的编队设计方法，即调整环绕卫星的半长轴。
The numerical computation for the secular variable of the semi - major axis , solar distance at perihelion , orbital periods and longitude of perihelion has been made for fifteen meteor streams by using the solution of gylden - meshcherckii equations
利用g - m型变质量天体轨道根数变化方程的一阶和二阶解对15个流星群轨道半长轴、近日点距离、轨道周期和近日点经度因太阳质量损失造成的每世纪的长期改变效应做了数值计算，并得出计算结果。
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。
The results show that the solar mass - loss extends the semi - major axis , the distance at perihelion and orbital periods of the meteor streams , especially , the extensive influence on the semi - major axis is not overlooked , but this influence on other orbital elements may be neglected
其计算结果表明，太阳质量损失使流星群轨道半长轴每世纪的改变效应较明显，它们同太阳距离的扩大影响值得关注，但对轨道周期的拉长每世纪的影响甚小，对近日点经度只有量级变化小到可以略而不计。
Our results show that , during the evolution of a binary system , the system widens as it loses mass , and the orbital period increase , while orbital eccentricity remains nearly constant , which can explain the distribution regulation of orbital elements of normal g - k giant and barium stars and the distribution character of the heavy - element abundances of barium stars
计算结果表明，随着星风吸积过程的进行，在星风质量损失阶段系统轨道半长轴将增大，导致轨道周期增大，而偏心率变化不大，由此可以解释普通红巨星双星系统和钡星系统的轨道根数的分布规律和变化情况以及钡星重元素丰度分布特征。