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661.
三维捷联磁传感器误差分析及补偿 总被引:2,自引:1,他引:1
磁传感器在导航系统中的应用日益广泛。在车载导航系统工作环境中,外界干扰磁场复杂,严重影响了磁航向测量的精度。因此对磁航向进行适当的罗差补偿是提高磁航向测量精度的有效途径。文中介绍了用磁传感器进行磁航向测量的原理,分析了由于磁场矢量叠加产生的罗差,提出了基于傅立叶级数的罗差模型和补偿方法。工程实践表明,上述方法的使用收到了较好的效果。 相似文献
662.
航天器空间动态磁场模拟技术 总被引:1,自引:0,他引:1
文章论述了卫星空间动态磁场模拟技术的原理和方案,阐述了对方案的工程化实现所进行的必要计算及对系统的各个部分所进行的研究设计。在此基础上建立了一套动态磁场模拟系统,为卫星空间动态磁场模拟试验提供了条件。 相似文献
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电磁脉冲武器已在现代战争中崭露头角,它的出现为抗击空袭飞机(包括隐身飞机)提供了一条新的思路。在分析电磁脉冲武器特点和国内外电磁脉冲武器研究进展的基础上,论述了电磁脉冲武器抗击来袭飞机(包括隐身飞机)的可行性和方法。 相似文献
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N.L. Borodkova J.B. Liu Z.H. Huang G.N. Zastenker 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(8):1220-1225
We present a comparison of large and sharp solar wind dynamic pressure changes, observed by several spacecraft, with fast disturbances in the magnetospheric magnetic field measured by the GOES-8, 9 and 10 geosynchronous satellites. Almost 400 solar wind pressure changes in the period 1996–2003 were selected for this study. Using the large statistics we confirmed that increases (decreases) in the dynamic pressure always results in increases (decreases) in the magnitude of geosynchronous Bz component. The amplitude of the geosynchronous Bz response strongly depends on the location of observer relative to the noon meridian, from the value of solar wind pressure before the disturbance arriving and firstly – from the amplitude of the pressure change. 相似文献
669.
Solar magnetic field is believed to play a central role in solar activities and flares, filament eruptions as well as CMEs
are due to the magnetic field re-organization and the interaction between the plasma and the field. At present the reliable
magnetic field measurements are still confined to a few lower levels like in photosphere and chromosphere. Although IR technique
may be applied to observe the coronal field but the technique is not well-established yet. Radio techniques may be applied
to diagnose the coronal field but assumptions on radiation mechanisms and propagations are needed. Therefore extrapolation
from photospheric data upwards is still the primary method to reconstruction coronal field. Potential field has minimum energy
content and a force-free field can provide the required excess energy for energy release like flares, etc. Linear models have
undesirable properties and it is expected to consider non-constant-alpha force-free field model. As the recent result indicates
that the plasma beta is sandwich-ed distributed above the solar surface (Gary, 2001), care must be taken in modeling the coronal
field correctly. As the reconstruction of solar coronal magnetic fields is an open boundary problem, it is desired to apply
some technique that can incorporate this property. The boundary element method is a well-established numerical techniques
that has been applied to many fields including open-space problems. It has also been applied to solar magnetic field problems
for potential, linear force-free field and non-constant-alpha force-free field problems. It may also be extended to consider
the non-force-free field problem. Here we introduce the procedure of the boundary element method and show its applications
in reconstruction of solar magnetic field problems.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
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