基于FM—AM转换的伪码调相-载波调频复合引信信号的脉内特征提取研究

伪码调相和载波调频复合信号因具有好的距离、速度分辨率和测速测距精度，所以广泛应用在雷达和引信中。在电子对抗中为了实施欺骗性干扰，必须有效地提取复合信号的参数特征，为此本文研究了FM-AM转换时频分析的理论及其实现方法，并利用该方法对伪码调相-载波调频复合信号进行了脉内特征分析。具体包括伪码调相正弦载波信号、伪码调相复合正弦调频信号及伪码调相复合线性调频信号。仿真结果表明，在信噪比为5dB时，利用FM—AM转换时频分析技术，不但可以提取载波调频的特征信息，而且能够有效提取伪码的特征信息。     

1773光纤数据总线技术与应用研究

讨论了4种光调制技术,利用其中的一种最优方法设计了基于1553B/1773总线的网关电路,并组成含4个站点的无源星型网络拓扑结构的1773总线多路数据传输网进行试验验证。试验结果表明,以光纤替代屏蔽双绞线作为传输介质的1773光纤数据总线能够使1553B总线系统具有更强的性能和更高的可靠性。     

空间太阳能发电和微波与电离层相互作用

本文第一部分研究了空间太阳能热发电，基于所提的评价动力系统的准则，比较了三种热力学系统，并给出了一些参数变化对闭式回热Ｂｒａｙｔｏｎ循环系统的影响，本文第二部分对微波速对电离层中电子的加速和受热进行了数值研究，得出了一些结果。     

基于AD9954芯片的非线性调频信号实现

提出了一种基于新型直接式数字合成(DDS)AD9954芯片,用数字阶梯逼近法直接读取数据产生非线性调频(NLFM)信号的方法。介绍了NLFM信号的实现、PIC控制电路与接口,分析了方法的不足。研究表明,该法所用硬件资源少,适于小时宽频宽乘积的非线性调频脉冲信号的实现。     

Implications of a weak termination shock

Recent observations from the Voyager spacecraft have suggested that the spectrum of the anomalous cosmic ray component is relatively steep at the termination shock, which is believed to be responsible for accelerating these particles. This conclusion argues that the termination shock must be weak, which in turn requires that the upstream Mach number in the solar wind must be quite low, 2.4. It is pointed out that such conditions are unlikely to prevail at all locations along the shock front. However, it is possible for such conditions to exist at the interface between high speed streams at high heliographic latitudes and the region at low latitudes where high and low speed streams have interacted and come into equilibrium. This discussion suggests a preferred location for the injection of the anomalous component into the shock acceleration process.     

调频光外差光纤位移传感器响应速度的研究

对调频光外差光纤位移传感器的动态响应速度进行了理论分析和实验论证。实验结果表明：调频光外差光纤位移传感器响应速度的提高，可通过增大调制频率和利用拍频信号的高次谐波成分来实现。     

Energy flux in the Earth's magnetosphere: Storm – substorm relationship

Three ways of the energy transfer in the Earth's magnetosphere are studied. The solar wind MHD generator is an unique energy source for all magnetospheric processes. Field-aligned currents directly transport the energy and momentum of the solar wind plasma to the Earth's ionosphere. The magnetospheric lobe and plasma sheet convection generated by the solar wind is another magnetospheric energy source. Plasma sheet particles and cold ionospheric polar wind ions are accelerated by convection electric field. After energetic particle precipitation into the upper atmosphere the solar wind energy is transferred into the ionosphere and atmosphere. This way of the energy transfer can include the tail lobe magnetic field energy storage connected with the increase of the tail current during the southward IMF. After that the magnetospheric substorm occurs. The model calculations of the magnetospheric energy give possibility to determine the ground state of the magnetosphere, and to calculate relative contributions of the tail current, ring current and field-aligned currents to the magnetospheric energy. The magnetospheric substorms and storms manifest that the permanent solar wind energy transfer ways are not enough for the covering of the solar wind energy input into the magnetosphere. Nonlinear explosive processes are necessary for the energy transmission into the ionosphere and atmosphere. For understanding a relation between substorm and storm it is necessary to take into account that they are the concurrent energy transferring ways. This revised version was published online in August 2006 with corrections to the Cover Date.     

SOHO: The Solar and Heliospheric Observatory

The Solar and Heliospheric Observatory (SOHO), together with the Cluster mission, constitutes ESA's Solar Terrestrial Science Programme (STSP), the first Cornerstone of the Agency's long-term programme Space Science — Horizon 2000. STSP, which is being developed in a strong collaborative effort with NASA, will allow comprehensive studies to be made of the both the Sun's interior and its outer atmosphere, the acceleration and propagation of the solar wind and its interaction with the Earth. This paper gives a brief overview of one part of STSP, the SOHO mission.     

Radio Diagnostics of the Solar Flare Reconnection

First, high-frequency (HF) slowly drifting pulsating structures are interpreted as radio emissions of electron beams accelerated in the magnetic reconnection volume and injected into magnetic islands (plasmoids). Then, the time evolution of plasma parameters (density, magnetic field, etc.) in a 2-D MHD model of solar flare reconnection is computed numerically. Assuming plasma radio emission from locations where the “double-resonance’’ instability generates upper-hybrid (UH) waves due to unstable distribution function of suprathermal electrons, the radio spectra and spatial source structures in the reconnection region are modeled. By comparison of the modeled and observed spectra a remarkable similarity has been found between the computed narrow-band emission and the observed lace bursts. Finally, a new diagnostics of the reconnection process is proposed.     

卫星太阳电池阵的刚-柔耦合动力学

研究了卫星太阳电池阵在多点撞击过程中的刚-柔耦合动力学问题．基于Jourdain速度变分原理和单向递推组集方法，建立了柔性多体系统的动力学模型．用Hertz撞击法则建立了撞击力和撞击处的局部变形关系，分别用刚体模型和柔性体模型仿真计算了太阳电池阵的撞击力、撞击时间，揭示了变形运动和大范围运动的相互耦合作用．