Free librations of the two-layer Moon and the possibilities of their detection

Based on the forthcoming second stage of the Japanese Lunar mission ILOM (2013), when an optical telescope will be set on the surface near one of the Lunar poles, the possibility to detect free Lunar modes (Chandler-like wobble and free-core nutation) is considered. The difference between the Lunar Eulerian and Chandler-like wobble is explained. The terms “arbitrary libration” and “free libration” are discussed. The geometrical and physical interpretations of the free polar motion over the Lunar surface are considered from the viewpoints of Lunar surface-based observations and the Lunar Navigation Almanac. The dependencies of the free libration period on the core’s radius, density, and ellipticity are modelled and discussed.     

极区中层夏季回波与频率关系的初步分析

研究不同频率的雷达体在不同时间和地点测量的极区中层夏季回波(Polar Mesosphere Summer Echoes,PMSE)体反射率,发现雷达体反射率与工作频率的4次方成反比,即产生PMSE回波的散射体的雷达散射截面与频率的4次方成反比,这种频率依赖关系不同于传统湍流理论.最后提出了PMSE实验和理论研究的新方法.      

超声速光学头罩流场的PIV研究

在马赫数Ma-3．8超声速风洞中,采用PIV（Particle Image Velocimetry,粒子图像测速）技术测量了超声速光学头罩流场的速度分布。PIV技术应用于超声速流场时,对系统的硬件配备、示踪粒子的跟随性以及PIV算法的精度有很高的要求。本文PIV系统选用高精度的同步控制器和高能量激光器;以纳米级粒径的粒子作为示踪粒子,通过斜激波响应实验分析了其在超声速流场中的跟随性;并采用多种高精度速度场算法对粒子图像进行处理。实验结果表明,示踪粒子在超声速流场中有很好的跟随性,采用的高精度速度场算法能够很好地反映超声速光学头罩流场的速度分布。     

Study on solar sources and polar cap absorption events recorded in Antarctica

Particularly intense events occurred on the Sun in a period around minimum of solar activity during cycle 23. We investigated the characteristics of September 2005 and December 2006 events and the properties of the correlated observations of ionospheric absorption, obtained by a 30 MHz riometer installed at Mario Zucchelli Station (MZS-Antarctica), and of geomagnetic activity recorded at Scott Base (Antarctica). Solar events are studied using the characteristics of CMEs measured with SoHO/LASCO coronagraphs and the temporal evolution of solar energetic protons in different energy ranges measured by GOES 11 spacecraft.     

行扫描光学遥感器扫描参数对遥感图像定位结果影响模型

定量分析了定位模型中输入参数误差与定位误差关系,提出了一种结果的校正方法。根据图像定位结果实际的偏离规律选择定位模型中能校正该偏离的参数,修改该参数达到校正定位结果以实现精准定位。建立了极轨气象卫星行扫描光学遥感仪器的像元定位数学模型,分析了遥感器扫描参数偏差对定位结果的影响,给出了定量的定位偏差计算公式,为遥感器定位结果的校正提供了理论模型,可为遥感器设计的误差控制提供参考。     

Multi-instrument observations of large-scale atmospheric gravity waves/traveling ionospheric disturbances associated with enhanced auroral activity over Svalbard

This study reports on observations of large-scale atmospheric gravity waves/traveling ionospheric disturbances (AGWs/TIDs) using Global Positioning System (GPS) total electron content (TEC) and Fabry–Perot Interferometer’s (FPI’s) intensity of oxygen red line emission at 630?nm measurements over Svalbard on the night of 6 January 2014. TEC large-scale TIDs have primary periods ranging between 29 and 65?min and propagate at a mean horizontal velocity of $～$749–761?m/s with azimuth of $～$345–347$°$ (which corresponds to poleward propagation direction). On the other hand, FPI large-scale AGWs have larger periods of $～$42–142?min. These large-scale AGWs/TIDs were linked to enhanced auroral activity identified from co-located all-sky camera and IMAGE magnetometers. Similar periods, speed and poleward propagation were found for the all-sky camera ($～$60–97?min and $～$823?m/s) and the IMAGE magnetometers ($～$32–53?min and $～$708?m/s) observations. Joule heating or/and particle precipitation as a result of auroral energy injection were identified as likely generation mechanisms for these disturbances.     

基于先验误差模型的机载高分宽幅DBF-SAR自聚焦算法

高分宽幅（HRWS）数字波束形成（DBF）合成孔径雷达（SAR）利用多通道空间采样代替部分时域采样,可以有效缓解SAR成像时高分辨率与宽测绘带间的矛盾,具有重要的军用和民用价值。现有常规DBF-SAR成像算法都假设雷达传感器相对位置精确已知,实际应用中受传感器位置测量误差影响,由位置不精确导致的相位误差会严重影响DBF-SAR高精度成像能力。在极坐标格式算法（PFA）框架下,推导了DBF-SAR成像处理后,残留相位误差的解析模型,分析了该误差对成像质量的影响。依据推导的先验相位误差解析结构模型,提出了一种基于图像对比度最优化准则的自聚焦算法。新算法通过引入先验相位结构信息,极大降低了待估参数的空间维数,可以同时改善自聚焦算法的参数估计精度和计算效率。数据处理结果验证了理论分析的正确性和所提算法的有效性。     

双麦克斯韦分布下极区中层尘埃粒子带电研究

在大功率微波照射下,极区中层夏季回波（PMSE）会立刻消失,该现象被称为极区中层加热现象.在大功率微波照射极区中层时,电子在微波电场加速下产生的定向运动速度与热运动速度可以比拟,极区中层的尘埃等离子体服从双麦克斯韦分布.基于双麦克斯韦分布下尘埃粒子充电理论给出极区中层尘埃粒子的电荷分布,比较了大功率微波对极区中层加热前和加热时,尘埃粒子电荷以及极区中层电子浓度的变化.结果表明,采用大功率微波装置加热极区中层会影响电子对尘埃粒子的充电进而导致电子浓度变化,这对解释极区中层加热现象具有重要意义.      

Interplanetary magnetic field control of plasma distribution in the polar ionosphere

We used the TEC (Total electron content) data of 5 min resolution obtained from the Madrigal database during solar-maximum winter (Nov. 6, 2000–Feb. 4, 2001) to study statistically the polar ionospheric plasma distribution response to different intensity and orientation of IMF By/Bz components. The sunlit high-density plasma extension from dayside to nightside is favored in negative IMF By and Bz conditions. With the magnitude of the negative Bz increasing, the time range corresponding to the distinct high-density extension feature expands, and the plasma density along the extension path enhances, which can be attributed to the interaction between dayside solar-produced ionization whose poleward limit is decided by terminator and convection extent mainly modulated by IMF Bz component. As for IMF By component influence on the sunlit plasma extension, the combination effect of convection and corotation electric fields is necessary to be considered.     

Old tail lobes effect on the solar-wind – Magnetosphere energy transport for the 27 August 2001 substorm

The magnetic flux of tail lobes Ψ is divided in two parts of comparable values Ψ₁ and Ψ₀₂, with the first that appears during substorm and the second, observed before substorm start. The first was named “new magnetic flux”, the second – “old magnetic flux”. The first, Ψ₁, is known to play a definitive role in the energy transport from the solar wind into the magnetosphere-ionosphere-atmosphere system, but the role of Ψ₀₂ in this transport is not well known. From the 27 August 2001 substorm data we study the involvement in the above transport process of the old flux Ψ₀₂. This involvement is observed in the polar cap (PC) area, which existed prior to the substorm and is called respectively “the old PC”. In this study, as distinct from earlier works, we use the balance equation of the energy stored in magnetosphere and energy consumed. Activation of the old PC magnetic flux Ψ₀₂ was found to increase the energy input by ∼85% in the event under consideration.