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径向脉动
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  “径向脉动”译为未确定词的双语例句
     Amplitude Variations of the Multimode Nonradial δ Scuti Pulsator 4 CVn
     盾牌座δ型变星4CVn的多重非径向脉动振幅变化
短句来源
     Simulation results show that bubbles induce the circulation of particles in the fluidized bed in which the distribution of particle velocities can be expressed by the Gauss distribution.
     计算结果表明床内气泡的形成造成床内颗粒的循环,使得流化床内颗粒具有不同的轴向和径向脉动速度,颗粒分速度分布近似服从高斯分布。
短句来源
     Nonradial Pulsations of Very Hot Dwarf Stars
     甚热矮星的非径向脉动
短句来源
     DECOUPLING TREATMENT OF LINEAR NONADIABATIC NONRADIAL PULSATIONS OF STARS
     恒星线性非绝热非径向脉动问题的退耦化处理方法
短句来源
     Nonradial Pulsation of stars and Its Mode Identification
     恒星的非径向脉动和模式证认
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  相似匹配句对
     Nonradial Pulsations of Very Hot Dwarf Stars
     甚热矮星的非径向脉动
短句来源
     Nonradial Pulsation of stars and Its Mode Identification
     恒星的非径向脉动和模式证认
短句来源
     Radial Bogis
     径向转向架
短句来源
     Plunge-cut gear-shaving process
     径向剃齿
短句来源
     Chaotic Pulsation in Variable Stars
     变星的混沌脉动
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  radial pulsation
At constant luminosity-to-mass ratio, the radial pulsation period is determined only by the effective temperature of the star.
      
For a perfect gas disk with γ= 5/3 the disk is stable with frequency (MG/r3)1/2 for purely radial pulsation with expanding and contracting boundary.
      
The effect of internal noise on the response characteristics of nonlinear radial pulsation in polytropic model has been investigated using the equivalent linearization technique.
      
The theory of radial pulsation predicts the trend of this correlation.
      
The period ratio ofP1/P0=0.762 indicates radial pulsation.
      
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In this paper, we develope a decoupling method to deal with linear nonadiabatic non-radial pulsations of stars. We decompose the sixth order differential equations of linear nonadiabatic nonradial pulsation into a fourth order differential equation and a second order differential equation. These two equations are linked by an algebraic equation. The decoupling treatment overcomes such difficulties as small domain and slow speed of convergence encountered in numerically solving the differential equations of the...

In this paper, we develope a decoupling method to deal with linear nonadiabatic non-radial pulsations of stars. We decompose the sixth order differential equations of linear nonadiabatic nonradial pulsation into a fourth order differential equation and a second order differential equation. These two equations are linked by an algebraic equation. The decoupling treatment overcomes such difficulties as small domain and slow speed of convergence encountered in numerically solving the differential equations of the problem, and naturally provides a guess solution which is needed in Henyey method.

本文发展了一种解恒星线性非绝热非径向脉动问题的退耦化方法。这个方法把非绝热非径向脉动问题的六阶线性微分方程,分解为由一个代数方程联系起来的一个四阶线性微分方程和另一个二阶线性微分方程进行数值求解。这样的一个退耦处理,有利于克服以前在数值解这类问题时常常遇到的收敛域小和收敛速度慢等困难,并且为数值解方程时所采用的Henyey方法提供了一个自然和方便的初始猜测解。

A multi-period analysis has been conducted on the data set of BDS 1269 A made up of the observations obtained by Percy and Rucihski during October 9 to November 6, 1976. In our period analysis, many possible frequencies, which include all frequencies suspected, are selected to constitute the initial frequency estimates. By fitting various combinations of the initial frequencies to the data set, the best one can be determined, which has a minimum number of different frequencies with the lowest residuals. The...

A multi-period analysis has been conducted on the data set of BDS 1269 A made up of the observations obtained by Percy and Rucihski during October 9 to November 6, 1976. In our period analysis, many possible frequencies, which include all frequencies suspected, are selected to constitute the initial frequency estimates. By fitting various combinations of the initial frequencies to the data set, the best one can be determined, which has a minimum number of different frequencies with the lowest residuals. The best fitting frequency solution includes f1=6.22999 cycle d-t, f2 = 6.50840 cycle d-1, f3 = 11.77324 cycle d-1, f4= 9.71369 cycle d-1 and f3= 11.33694 cycled-1. The numeric experiment justifies this five-frequency solution. Based on this solution, a reasonable non-radial rotational splitting pulsation mode is identified, and a rotational velocity v3 = 30 km s-1 is predicted, which tends to agree with the fact that BDS 1269 A is a slowly rotational star.A total of 459 new measurements of four nights during 1987 October 16 to 24 were taken by authors with a Johnson V filter. The fitting with the five-frequency solution to the new data is very good with a residual which is near the uncertainty of the observation.

以同一参考系归化Percy及Rucinski在1976年10月9日至11月6日获得的BDS1269A的光电测光数据后,利用多重周期分析方法进行周期分析,在周期初值的选取中尽可能穷尽所有可能的组合,最后根据最小残差获得最佳组合.我们认为BDS 1269 A的最佳频率解为:f_1=6.22999周每天,f_2=6.50840周每天,f_3=11.77324周每天,f_4=9.7136周每天,f_5=11.33694周每天.反证实验证明这组频率是充分的.基于以上频率解,一个非径向脉动目转分裂模型得以建立,其预言的自转速度。v_6=30km s~(-1)与BDS 1269A是一颗低速自转恒星的观测结果相吻合. 1987年10月16日至24日,我们取得了BDS1269 A的459个新的V波段光电观测点.上述频率解拟合此数据结果很好,拟合残差与观测误差一致.频率解得到了一次验证.

Today, rapidly oscillating Ap (roAp) stars are one kind of most principal objects in the asteroseismologic study, which exhibit nonradial p-modes pulsations with very high overtone. As ideal targets for the new techniques of asteroseismology, analyses of roAp oscillations are yielding valuable, even unique information about magnetic peculiar stars. By comparing observed frequency spectrum to asymptotic pulsation theory, we can investigate diverse properties of roAp stars, radius, rotation period, evolutionary...

Today, rapidly oscillating Ap (roAp) stars are one kind of most principal objects in the asteroseismologic study, which exhibit nonradial p-modes pulsations with very high overtone. As ideal targets for the new techniques of asteroseismology, analyses of roAp oscillations are yielding valuable, even unique information about magnetic peculiar stars. By comparing observed frequency spectrum to asymptotic pulsation theory, we can investigate diverse properties of roAp stars, radius, rotation period, evolutionary status, the geometry and internal strength of magnetic field; and, potentially, the detailed temperature structure of the atmosphere. In this paper, the discovery of roAp stars and their basic data are reveiwed. The general characteristics of Ap stars and the oblique rotator model, also, the general characteristics of roAp stars and the oblique pulsator model, are introduced. In addition, the excitation mechanisms and recent research developments of roAp stars are discussed.

快速振荡的Ap星(roAp),作为高阶P模式非径向脉动的主序星,已成为星震学研究的主要目标之一。通过对roAp星振荡的分析,可以获取磁Ap星有价值的、甚至唯一的资料。可以研究roAp星的半径、自转周期、演化态、大气结构,甚至恒星内部磁场等等。本文综述了roAp星的发现及其现有基本数据,介绍了Ap星的一般特点与倾斜转子模型,介绍了roAp星的一般特点与倾斜脉动模型。讨论了roAp星的激发机制以及最新的研究发展。

 
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