1) magnetar
磁星
1.
Several theoretical models of SGRs are briefly introduced, among them the magnetar (neutron star with ultra strong magnetic field) model accounts for their observations fairly well.
对SGRs的主要观测特征———在软伽玛射线波段的重复爆发及持久性的周期的X射线辐射———进行了回顾 ,介绍了SGRs的一些理论模型 ,其中磁星 (具有甚强磁场的中子星 )模型较合理地解释了现有的观测事
2) satellite magnetic survey
卫星磁测
1.
Following 20-years long silence in satellite magnetic survey after POGOs in1967～1971 and MAGSAT in 1979～1980,the magnetic satellites Orsted,Champ and SCAC were launched in February 1999,July and November,2000 by Denmark,Germany and Argentina,respectively.
自此之后,卫星磁测沉静了20年。
3) Electromagnetic satellite
电磁卫星
1.
It is still an unsolved question how the electromagnetic anomalies observed on the electromagnetic satellite move from the Lithosphere to the ionosphere or the aerosphere.
对于电磁卫星所观测到的地震震前电磁异常现象的机制,即电磁异常如何从岩石圈穿过大气层耦合到电离层及其以上空间,目前仍是尚未解决的问题。
2.
On the basis of the requirement for earthquake monitoring and GPS obscuration observation technology, an electromagnetic satellite constellation is designed by figure simulation and Genetic Algorithms.
根据地震监测任务对电磁卫星的需求,利用点数字仿真方法和遗传算法优化设计了电磁卫星星座。
3.
On May 9,3 days before the earthquake,many local electromagnetic perturbations were detected by geomagnetic low point displacement,total electron concentration(TEC)inversed by GPS observation,foF2 obtained by ionospheric sounding and ion density and temperature detected by electromagnetic satellite,with most amplitude exceeding 50%.
2%,同时多台电阻率观测在震前1个月左右显示短临突变异常;震前18天地磁垂直分量出现低点位移,分界线两侧的低点时间超过2h;震前3天即5月9日,地磁低点位移、利用GPS反演得到的电离层总电子含量(TEC)、电离层测高仪得到的foF2和电磁卫星监测的离子密度和温度等均观测到局部电磁扰动现象,多数异常幅度超过50%。
4) magnetic satellite
磁测卫星
5) magnetic neutron star
磁中子星
1.
Adopting electron cyclotron resonance absorption coefficient in semi classic quantum theory,using radiation transfer equation,we calculated the radiation spectra across the plasma near magnetic neutron star,and found it accords well with the observation spectra of GRB.
运用半经典量子理论的电子回旋共振吸收系数 ,由辐射转移方程计算了通过磁中子星表面附近等离子体后的辐射谱 ,与 γ射线暴的观测谱符合得很好 。
6) satellite magnetic moment
卫星磁矩
补充资料：磁星
| 磁星 magnetic star 具有强磁场的恒星。通常光谱型为A，磁场可以强到3特(斯拉)。磁星的磁场强度还在变化，故又称磁变星。磁变星大多为A型特殊星。一部分磁变星，不仅磁场周期性变化，光度和光谱也变化。光变周期1～25天，变幅一般不超过0.1等，典型星是猎犬座a2(常陈一)，在5.469天周期内，磁场强度从+0.162特变0.142特，亮度改变0.1等。光谱变化表现为一些谱线的强度有规则的变化，特别是铬和铕的谱线。有些磁变星磁场与光度同相变化，另一些则相反。按照斜转子模型，磁轴对自转轴有较大倾斜，假定不同元素由于某种尚不清楚的原因聚集在星面上不同区域，随着自转，星面上磁场和元素分布不同的区域，随着自转，星面上磁场和元素分布不同的区域轮流朝向观测者，便观测到磁场和光谱的周期性变化。 |
说明：补充资料仅用于学习参考，请勿用于其它任何用途。
参考词条