助手标题  
全文文献 工具书 数字 学术定义 翻译助手 学术趋势 更多
查询帮助
意见反馈
   旋转中子星 在 天文学 分类中 的翻译结果: 查询用时:1.582秒
图标索引 在分类学科中查询
所有学科
天文学
数学
更多类别查询

图标索引 历史查询
 

旋转中子星
相关语句
  rotating neutron stars
    Comparison of Two Methods for Calculating Properties of Rotating Neutron Stars
    两种计算旋转中子星性质方法的比较(英文)
短句来源
  “旋转中子星”译为未确定词的双语例句
    Two numerical schemes of rotational neutron star based on general relativity, Hartle code and Butterworth and Ipser’s code(BI code), are introduced and discussed.
    对两种基于广义相对论的计算旋转中子星性质的数值方法: Hartle法和Butterworth和Ipser法(简记为BI法)进行了较详细的介绍、讨论和比较.
短句来源
    The numerical results of the two codes with different equations of state(EOSs) are compared, and the results indicate that most properties of rotational neutron star with different EOSs and different numerical schemes are in accordance with each other.
    对基于不同物态方程给出的旋转中子星的性质进行对比, 结果表明两种方法给出的相关结果例如旋转中子星的质量、半径和形变等基本一致, 特别是在观测值范围内的计算等均能较好地解释观测结果
短句来源
    Two numerical schemes of rotational neutron star based on general relativity, Hartle code and Butterworth and Ipser' s code(BI code), are introduced and discussed. The numerical results of the two codes with different equations of state(EOSs) are compared, and the results indicate that most properties of rotational neutron star with different EOSs and different numerical schemes are in accordance with each other.
    对两种基于广义相对论的计算旋转中子星性质的数值方法:Hartle法和Butterworth和 Ipser法(简记为BI法)进行了较详细的介绍、讨论和比较.对基于不同物态方程给出的旋转中子星的性质进行对比,结果表明两种方法给出的相关结果例如旋转中子星的质量、半径和形变等基本一致,特别是在观测值范围内的计算等均能较好地解释观测结果.
查询“旋转中子星”译词为用户自定义的双语例句

    我想查看译文中含有:的双语例句
例句
为了更好的帮助您理解掌握查询词或其译词在地道英语中的实际用法,我们为您准备了出自英文原文的大量英语例句,供您参考。
  rotating neutron star
Energy release during disk accretion onto a rapidly rotating neutron star
      
Based on the static criterion for stability, we present a method of constructing the dependence of gravitational mass M on Kerr rotation parameter j and on total baryon mass (rest mass) m for a rigidly rotating neutron star.
      
Energy release on the surface of a rapidly rotating neutron star during disk accretion: A thermodynamic approach
      
Expressions are derived for the energy release during accretion onto a cool (with constant entropy), rapidly rotating neutron star (NS) in the Newtonian theory and in general relativity.
      
The results obtained are used for analysis in terms of the transition-layer model (TLM) and the relativistic-precession model (RPM) for a slowly rotating neutron star.
      
更多          
  rotating neutron star
Energy release during disk accretion onto a rapidly rotating neutron star
      
Based on the static criterion for stability, we present a method of constructing the dependence of gravitational mass M on Kerr rotation parameter j and on total baryon mass (rest mass) m for a rigidly rotating neutron star.
      
Energy release on the surface of a rapidly rotating neutron star during disk accretion: A thermodynamic approach
      
Expressions are derived for the energy release during accretion onto a cool (with constant entropy), rapidly rotating neutron star (NS) in the Newtonian theory and in general relativity.
      
The results obtained are used for analysis in terms of the transition-layer model (TLM) and the relativistic-precession model (RPM) for a slowly rotating neutron star.
      
更多          
  rotating neutron stars
Models are constructed for rapidly rotating neutron stars, which could form after the collapse of rotating iron cores of evolved massive stars.
      
As the changes of the mass and radius of a real neutron star caused by rotation are very small in comparison with the total mass and radius, one can see that Hartle's approximate method is rational to deal with the rotating neutron stars.
      
This review describes the observational properties of radio pulsars, fast rotating neutron stars, emitting radio waves.
      
The resulting theory has applications both to rotating helium II in the laboratory, and to rotating neutron stars (pulsars).
      
Searching for gravitational waves from rotating neutron stars
      
更多          


Two numerical schemes of rotational neutron star based on general relativity, Hartle code and Butterworth and Ipser’s code(BI code), are introduced and discussed. The numerical results of the two codes with different equations of state(EOSs) are compared, and the results indicate that most properties of rotational neutron star with different EOSs and different numerical schemes are in accordance with each other.

对两种基于广义相对论的计算旋转中子星性质的数值方法: Hartle法和Butterworth和Ipser法(简记为BI法)进行了较详细的介绍、讨论和比较. 对基于不同物态方程给出的旋转中子星的性质进行对比, 结果表明两种方法给出的相关结果例如旋转中子星的质量、半径和形变等基本一致, 特别是在观测值范围内的计算等均能较好地解释观测结果

>=Two numerical schemes of rotational neutron star based on general relativity, Hartle code and Butterworth and Ipser' s code(BI code), are introduced and discussed. The numerical results of the two codes with different equations of state(EOSs) are compared, and the results indicate that most properties of rotational neutron star with different EOSs and different numerical schemes are in accordance with each other.

对两种基于广义相对论的计算旋转中子星性质的数值方法:Hartle法和Butterworth和 Ipser法(简记为BI法)进行了较详细的介绍、讨论和比较.对基于不同物态方程给出的旋转中子星的性质进行对比,结果表明两种方法给出的相关结果例如旋转中子星的质量、半径和形变等基本一致,特别是在观测值范围内的计算等均能较好地解释观测结果.

 
图标索引 相关查询

 


 
CNKI小工具
在英文学术搜索中查有关旋转中子星的内容
在知识搜索中查有关旋转中子星的内容
在数字搜索中查有关旋转中子星的内容
在概念知识元中查有关旋转中子星的内容
在学术趋势中查有关旋转中子星的内容
 
 

CNKI主页设CNKI翻译助手为主页 | 收藏CNKI翻译助手 | 广告服务 | 英文学术搜索
版权图标  2008 CNKI-中国知网
京ICP证040431号 互联网出版许可证 新出网证(京)字008号
北京市公安局海淀分局 备案号:110 1081725
版权图标 2008中国知网(cnki) 中国学术期刊(光盘版)电子杂志社