论赤道扩展F的密度不规则体(Ⅱ)

本文对等离子体中的电子和离子分别采用流体和动力论描述, 导出适于描述夜间赤道F层现象的若干非线性模型。由此证明赤道扩展F小尺度区域可存在大量偶极涡、孤子和孤子链等类型的密度不规则体。      

一种航天测控冗余跟踪弧段处理方法

随着在轨航天器的日益增多,测控资源的需求量也日益增大,因此,其使用效率也倍受关注。当航天器重要测控弧段安排多个测控设备进行全力跟踪时,很容易出现测控弧段搭接或完全被覆盖的情况。为有效利用现有测控资源,针对弧段搭接的情况,提出了一种基于冗余度评价函数的跟踪弧段处理方法,该方法在不降低跟踪总时长情况下,通过合理有效地配置测控资源,剔除了冗余跟踪弧段,提高了现有测控资源的使用效率。     

C/C-Cu复合材料的烧蚀形貌和烧蚀机理

以PAN预氧化纤维整体毡为增强体,经碳化、等温CVI致密化后制备多孔的C/C复合材料预制体,利用气体压力浸渗法将Cu引入C/C预制体中制备C/C-Cu复合材料。采用氢氧(H2-O2)焰考核C/C-Cu复合材料的烧蚀性能,经扫描电镜和电子能谱对不同烧蚀区域的微观结构和成分进行分析,结果表明:预制体密度为0.96 g/cm3的C/C-Cu复合材料的线烧蚀率和质量烧蚀率分别为4.75μm/s、0.223 mg/s,烧蚀性能优良;其烧蚀表面具有不同的宏观形貌,在烧蚀中心区产生了明显的凹坑,主要烧蚀机制为C/C预制体的氧化和铜基体的机械冲刷;烧蚀过渡区聚集了大量的铜基体,其烧蚀机制为Cu的热氧化和机械冲刷;烧蚀边缘区材料表面变黑,主要因为C/C的氧化。为了提高C/C-Cu的烧蚀性能,需要发挥C/C预制体的"钉扎"作用,阻止Cu在高温下被气流冲刷而发生流动。     

一种航天测控系统可靠性定量化计算方法

航天测控系统具有动态性、复杂性、可维修性、阶段间相关性等显著特征,作为航天器安全在轨运行的重要保障,其可靠性至关重要。针对航天测控系统可靠性精确计算的难点,提出了综合马尔可夫（Markov）模型和全概率思想的复杂、动态系统可靠性定量化计算方法,给出了计算流程。按照系统的动态组成特性,将任务进程划分为多个阶段,阶段内参试状态不变,不同阶段之间参试状态不同。借鉴Markov模型描述阶段内状态转移过程,通过求解Kolmogorov后向方程得到本阶段结束时的状态概率,利用全概率思想实现阶段间状态映射,体现阶段间的依赖性,依次对各阶段求解获取整个任务可靠性,具有求解准确度高、结果可信度高等特点。最后给出算例,通过与蒙特卡洛仿真结果的比对校验Markov方法的准确性。     

基于天通卫星系统的天基测控技术

针对卫星测控资源紧缺的现状,为满足未来大规模卫星用户对测控资源的使用便利性这一需求,研究利用天通卫星进行近地低轨卫星测控服务的能力。天通作为高轨移动通信卫星系统,具有传输实时方便、服务安全可靠和综合效费比高等多方面的特点。首先,分析了天通卫星对不同倾角、轨道高度卫星的测控覆盖时长,以及对载人航天任务空间站和火箭进行测控的服务能力。然后,基于天通民用系统现有的系统架构,详细介绍了天通系统支持低轨测控的系统改造方案以及工作流程。最后,结合目前的技术发展趋势和天通卫星能力现状,描述了天通卫星在天基测控和低速中继两种任务场景中的应用前景。     

多电飞机主发电机供电条件模拟装置设计

多电飞机主发电机要接入电网向电网供电,须要满足很多条件。首先要使准备接通的发电机励磁,然后当发电机转速正常,发电机电压达到要求后,并在外电源已经断开的条件下,接通发电机接触器,使发电机向电网供电。设计基于C8051单片机及外围电路的装置,对多电飞机主发电机接入电网的控制条件进行模拟,并将结果显示在装置的LCD(Liquid Crystal Display,简称LCD)显示屏上。该装置的设计包括硬件电路设计和软件程序编写。最后对装置进行调试与验证,实验结果能够达到设计初衷。     

Fundamental (f) oscillations in a magnetically coupled solar interior-atmosphere system – An analytical approach

Solar fundamental (f) acoustic mode oscillations are investigated analytically in a magnetohydrodynamic (MHD) model. The model consists of three layers in planar geometry, representing the solar interior, the magnetic atmosphere, and a transitional layer sandwiched between them. Since we focus on the fundamental mode here, we assume the plasma is incompressible. A horizontal, canopy-like, magnetic field is introduced to the atmosphere, in which degenerated slow MHD waves can exist. The global (f-mode) oscillations can couple to local atmospheric Alfvén waves, resulting, e.g., in a frequency shift of the oscillations. The dispersion relation of the global oscillation mode is derived, and is solved analytically for the thin-transitional layer approximation and for the weak-field approximation. Analytical formulae are also provided for the frequency shifts due to the presence of a thin transitional layer and a weak atmospheric magnetic field. The analytical results generally indicate that, compared to the fundamental value ($\omega =\sqrt{\mathit{gk}}$), the mode frequency is reduced by the presence of an atmosphere by a few per cent. A thin transitional layer reduces the eigen-frequencies further by about an additional hundred microhertz. Finally, a weak atmospheric magnetic field can slightly, by a few percent, increase the frequency of the eigen-mode. Stronger magnetic fields, however, can increase the f-mode frequency by even up to ten per cent, which cannot be seen in observed data. The presence of a magnetic atmosphere in the three-layer model also introduces non-permitted propagation windows in the frequency spectrum; here, f-mode oscillations cannot exist with certain values of the harmonic degree. The eigen-frequencies can be sensitive to the background physical parameters, such as an atmospheric density scale-height or the rate of the plasma density drop at the photosphere. Such information, if ever observed with high-resolution instrumentation and inverted, could help to gain further insight into solar magnetic structures by means of solar magneto-seismology, and could provide further insight into the role of magnetism in solar oscillations.     

Midlatitude ionospheric F2-layer response to eruptive solar events-caused geomagnetic disturbances over Hungary during the maximum of the solar cycle 24: A case study

In our study we analyze and compare the response and behavior of the ionospheric F2 and of the sporadic E-layer during three strong (i.e., Dst?<??100nT) individual geomagnetic storms from years 2012, 2013 and 2015, winter time period. The data was provided by the state-of the art digital ionosonde of the Széchenyi István Geophysical Observatory located at midlatitude, Nagycenk, Hungary (IAGA code: NCK, geomagnetic latitude: 46.17° geomagnetic longitude: 98.85°). The local time of the sudden commencement (SC) was used to characterize the type of the ionospheric storm (after Mendillo and Narvaez, 2010). This way two regular positive phase (RPP) ionospheric storms and one no-positive phase (NPP) storm have been analyzed. In all three cases a significant increase in electron density of the foF2 layer can be observed at dawn/early morning (around 6:00 UT, 07:00 LT). Also we can observe the fade-out of the ionospheric layers at night during the geomagnetically disturbed time periods. Our results suggest that the fade-out effect is not connected to the occurrence of the sporadic E-layers.     

Upgrading CCIR's foF2 maps using available ionosondes and genetic algorithms

We have developed a new approach towards a new database of the ionospheric parameter $f_{o}F2$. This parameter, being the frequency of the maximum of the ionospheric electronic density profile and its main modeller, is of great interest not only in atmospheric studies but also in the realm of radio propagation. The current databases, generated by CCIR (Committee Consultative for Ionospheric Radiowave propagation) and URSI (International Union of Radio Science), and used by the IRI (International Reference Ionosphere) model, are based on Fourier expansions and have been built in the 60s from the available ionosondes at that time. The main goal of this work is to upgrade the databases by using new available ionosonde data. To this end we used the IRI diurnal/spherical expansions to represent the $f_{o}F2$ variability, and computed its coefficients by means of a genetic algorithm (GA). In order to test the performance of the proposed methodology, we applied it to the South American region with data obtained by RAPEAS (Red Argentina para el Estudio de la Atmósfera Superior, i.e. Argentine Network for the Study of the Upper Atmosphere) during the years 1958–2009. The new GA coefficients provide a global better fit of the IRI model to the observed $f_{o}F2$ than the CCIR coefficients. Since the same formulae and the same number of coefficients were used, the overall integrity of IRI’s typical ionospheric feature representation was preserved. The best improvements with respect to CCIR are obtained at low solar activities, at large (in absolute value) modip latitudes, and at night-time. The new method is flexible in the sense that can be applied either globally or regionally. It is also very easy to recompute the coefficients when new data is available. The computation of a third set of coefficients corresponding to days of medium solar activity in order to avoid the interpolation between low and high activities is suggested. The same procedure as for $f_{o}F2$ can be perfomed to obtain the ionospheric parameter M(3000)F2.     

采用阵列天线的GPS接收机的多径抑制方法

提出一种新的用于阵列天线GPS接收机的多径抑制方法。考虑到通常GPS视线信号的来波方向与多径的来波方向不同,在每个导航数据符号位内测距（C/A）码重复,通过对阵列接收的信号矢量与它本身的延迟信号矢量互相关,提高接收机前端信噪比,再利用最大特征值法和前后向空间平滑技术准确地估计期望卫星视线信号（LOSS）的来波方向。最后综合多个GSC子阵列有效地降低了相关多径对码跟踪精度的影响。仿真结果显示,该方法能使接收机在与LOSS码同步前准确估计LOSS的角度信息,有效抑制相关多径,且鉴相结果准确。