引力势的英文

• attraction potential
• gravitational potential

• "引力"英文翻译    gravitation; gravitational f ...
• "势"英文翻译    power; force; influence
• "引力势，重力势" 英文翻译 :    gravitational potential
• "地引力势场" 英文翻译 :    earth potential field
• "引力势差" 英文翻译 :    gravitational potential difference
• "引力势能" 英文翻译 :    gravitation energy
• "引力势阱" 英文翻译 :    gravitarional potential well
• "引力势 重力势 重力位" 英文翻译 :    gravitationalpotential
• "引力势差，重力势差" 英文翻译 :    gravitational potential difference
• "引力势能，重力势能" 英文翻译 :    gravitational potential energy
• "力势" 英文翻译 :    force potential
• "引力" 英文翻译 :    [物理学] gravitation; gravitational force; attraction; attractive force 核引力 nuclear attraction; 万有引力 universal gravitation
• "动力势" 英文翻译 :    dynamic potential; power potential
• "热力势" 英文翻译 :    thermal potential; thermodynamic potential; thermodynamical potential; thermopotential
• "水力势" 英文翻译 :    hydraulic potential
• "压力势" 英文翻译 :    cyclic electron flow; pressure potential
• "重力势" 英文翻译 :    geopotential; gravitation potential; gravitational potential; gravity potential; gravitypotential; potential of gravitation; weight potential
• "地球重力势 地重力势 重力势" 英文翻译 :    geopotential
• "等重力势面" 英文翻译 :    surface of constant geopotential
• "地球重力势" 英文翻译 :    geopotential
• "地重力势" 英文翻译 :    geopotential
• "动力势差[位差]。" 英文翻译 :    dynamic elevation
• "动力势差数" 英文翻译 :    dynamical number
• "动力势高度" 英文翻译 :    dynamic height
• "非有心力势" 英文翻译 :    non central potential

• Properties of space must depend on the gravitational potential .
  空间性质一定与引力势有关。
• Gravitational potential difference
  引力势差
• Multiple closed orbits of fixed energy for 3 - body problems with gravitational potentials
  具有引力势的给定能量的三体问题的多个闭轨
• Besides , considering the differences of the galactic gravitational potential models , there is different influence for the distribution morphologies of all of the orbital parameters of the selected sample clusters
  此外，不同的银河系引力势模型对所选样本的轨道参数的分布形态也有不同程度的影响。
• ( 3 ) on basis of the result of equilibrium gravitating potential in a gravitational system , we explain the phenomenon of scale - free peculiar velocity in the universe by studying cosmic fluid equations . furthermore , we reexamine the issue in the approach of generalized statistical mechanics
  ( 3 )我们根据多体引力系统中得出的平衡引力势的形式，结合宇宙流体力学解释了ostriker提到的宇宙中速度与尺度无关( scale - free )的现象，并在广义统计力学范畴下进行了讨论。
• 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 。
• Haloes in the two accretion phases show systematically different properties , for example , the circular velocity vh increases rapidly with time and approximately equals the inner circular velocity vs in the fast accretion phase , but remain almost constant and less than vs in the slow accretion phase : the inner properties of a halo , such as rs and ms increase rapidly with time in the fast accretion phase but change only slowly in the slow accretion phase : the halo concentration changes slow in the fast accretion phase , but increases rapidly with the hubble expansion in the slow accretion phase . the inner structure and potential well associated with a halo is built up mainly in the fast accretion phase , while a large amount of mass can be accreted in the slow accretion phase without changing significantly the inner properties and the potential well
  ~ 4 ，其束缚能和具有相同圆周速度的等温球大致相等; ( s )在这两个阶段，暗晕的行为特征迥异(例如，圆周速度均‘在快速吸积阶段增长迅速且略大于内部圆周速度: 、 ，而在缓慢吸积阶段基本恒定甚至降低，且小于、 、 . : 、和呱在快速吸积阶段增长迅猛，而在缓慢吸积阶段增长滞缓) : ( l )一个暗晕的内部结构和引力势阱主要是在早期的快速吸积阶段成长起来的，虽然在缓慢增长阶段可以吸积大量的质量(超过10倍) ，但这并不显著地改变其内部特征和引力势阱
• 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。
• Finally the initial observational data are produced by monte carlo method , and the orbital parameters are calculated using the simulation data for the three sample clusters . the relationship between the distribution morphologies of the orbital parameters and the initial observational date as well as the different galactic gravitational potential models are discussed
  最后，对3个样本球状星团的观测数据进行montecarlo模拟，并用于计算它们的轨道参数，以及讨论轨道参数的分布形态与模拟观测数据和不同引力势模型之间的关系。

• 引力势的日语：じゅうりょくポテンシャル