Effects of sector structure of the interplanetary magnetic field on the upper mesosphere–lower thermosphere dynamics

In this paper we study the influence of the interplanetary magnetic field (IMF) polarity changes caused by the Earth passing through the IMF sector boundary on the dynamic processes taking place in neutral atmosphere within the altitude interval of the upper mesosphere–lower thermosphere (83–101 km). The analysis has revealed the influence of the IMF sector structure on dynamics of the upper mesosphere–lower thermosphere. There has been a significant seasonal variation of the wind reaction to the IMF polarity changes observed. The influence of the IMF polarity changes on neutral atmosphere dynamics within the altitude range of 83–101 km is most pronounced in the zonal component of neural wind when the IMF polarity changes from negative to positive in all the seasons except for spring and when IMF polarity changes from positive to negative – in spring only.     

Dependence of the 27-day variation of cosmic rays on the global magnetic field of the Sun

We show that the higher range of the heliolongitudinal asymmetry of the solar wind speed in the positive polarity period (A > 0) than in the negative polarity period (A < 0) is one of the important reasons of the larger amplitudes of the 27-day variation of the galactic cosmic ray (GCR) intensity in the period of 1995–1997 (A > 0) than in 1985–1987 (A < 0). Subsequently, different ranges of the heliolongitudinal asymmetry of the solar wind speed jointly with equally important corresponding drift effect are general causes of the polarity dependence of the amplitudes of the 27-day variation of the GCR intensity. At the same time, we show that the polarity dependence is feeble for the last unusual minimum epoch of solar activity 2007–2009 (A < 0); the amplitude of the 27-day variation of the GCR intensity shows only a tendency of the polarity dependence. We present a three dimensional (3-D) model of the 27-day variation of GCR based on the Parker’s transport equation. In the 3-D model is implemented a longitudinal variation of the solar wind speed reproducing in situ measurements and corresponding divergence-free interplanetary magnetic field (IMF) derived from the Maxwell’s equations. We show that results of the proposed 3-D modeling of the 27-day variation of GCR intensity for different polarities of the solar magnetic cycle are in good agreement with the neutron monitors experimental data. To reach a compatibility of the theoretical modeling with observations for the last minimum epoch of solar activity 2007–2009 (A < 0) a parallel diffusion coefficient was increased by ∼40%.     

Study of the 27-day variations of the galactic cosmic ray intensity and anisotropy

We demonstrate that the general features of the radial and azimuthal components of the anisotropy of galactic cosmic rays can be studied by the harmonic analysis method using data from an individual neutron monitor with cut off rigidity <5 GV. In particular, we study the characteristics of the 27-day (solar rotation period) variations of the galactic cosmic ray intensity and anisotropy, solar wind velocity, interplanetary magnetic field strength and sunspot number. The amplitudes of the 27-day variations of the galactic cosmic ray anisotropy are greater, and the phases more clearly established, in A > 0 polarity periods than in A < 0 polarity periods at times of minimum solar activity. The phases of the 27-day variations of the galactic cosmic rays intensity and anisotropy are opposite with respect to the similar changes of the solar wind velocity in A > 0 polarity periods. No significant dependence of the amplitude of the 27-day variation of the galactic cosmic ray anisotropy on the tilt angle of the heliospheric neutral sheet is found. Daily epicyclegrams obtained by Chree’s method show that the 27-day variations of the galactic cosmic ray anisotropy during A > 0 polarity periods follow elliptical paths with the major axes oriented approximately along the interplanetary magnetic field. The paths are more irregular during A < 0 polarity periods.     

Characteristics of the seasonal variation of the global tropopause revealed by COSMIC/GPS data

Using the Global Navigation Satellite System (GNSS) radio occultation observations from Formosa Satellite mission-3/Constellation Observing System for Meteorology, Ionosphere, and Climate (FORMOSAT-3/COSMIC) from 2007 to 2012, the climatological characteristics of the global tropopause was studied, with the following features identified. The overall results generally agree with previous studies. The tropopause has an obvious zonal structure, with more zonal characteristics in the Southern Hemisphere than the Northern Hemisphere. The vertical shape of the tropopause is sharp in the tropics and broad in the sub-tropical latitudes, with the sharpest latitudinal gradient in the mid-latitudes of both hemispheres. The global tropopause exists in a large range between 8 km and 17 km (or between 100 hPa and 340 hPa). The highest tropopause is over the South Asian monsoon regions for the entire year. The spatial structure of the tropopause in the polar region is of concentric structure, with an altitude between 7.5 km and 10 km. It is more symmetric in the Antarctic than the Arctic. Differing from other places, the height of the tropopause in the Antarctic is higher in winter as opposed to summer. The tropopause has distinct seasonal variability, especially in polar regions.     

Variations of geomagnetic cutoff rigidity in the southern hemisphere close to 70°W (South-Atlantic Anomaly and Antarctic zones) in the period 1975–2010

We report the existence of rapid variations in (effective) geomagnetic cutoff rigidity (Rc) between the equatorial and Antarctic zones adjacent to the Andes Mountains, revealed by the variation rate of geomagnetic cutoff rigidity (VRc) in the period 1975–2010. Our analysis is based on empirical records and theoretical models of the variations in cosmic rays and on the structure of geomagnetic fields. These have given us a different view of variations in Rc in time and space along the 70°W meridian, where secular variations in the geomagnetic field are strongly influenced by the proximity of the South Atlantic Magnetic Anomaly (SAMA), one of the most important characteristics of the terrestrial magnetic field that affects our planet, close from the equator to the 50°S parallel and from South America to South Africa. The VRc presents rapid changes in mid-latitudes where SAMA exerts its influence despite the existence of smooth changes in the geomagnetic field. This shows that these changes occur mainly in the spatial configuration, rather than in the temporal evolution of Rc. The analysis was performed using measurements from the Chilean Network of Cosmic Rays and Geomagnetism Observatories, equipped with BF-3 and latest generation He-3 neutron monitors, Fluxgate magnetometers, geomagnetic reference field (IGRF) and Tsyganenko 2001 model (just for completeness).     

基于流场/声爆耦合伴随方程的超声速公务机声爆优化

基于自主研发的大规模并行结构化网格CFD求解器PMB3D以及并行化伴随方程求解器PADJ3D，开展了流场/声爆伴随方程的求解研究。首先采用标准算例，对内部CFD代码PMB3D软件和声爆预测代码进行了声爆计算可信度验证，以及声爆强度对近场声压梯度的校核。针对并行环境下多块对接网格的近场声压提取操作的复杂性，提出了"包围盒"的方法实现并行环境下近场声压装配单元编号、网格块编号以及对应的进程编号确定，基于声爆计算坐标将并行传递的数据进行一维排序，为声爆预测、伴随方程以及梯度求解提供输入条件。通过线性插值雅克比矩阵实现均匀坐标系梯度信息向非均匀坐标转换，并进一步根据结构化网格特征提出了插值原则，简化了近场声压转换雅克比矩阵的变分。通过装配单元记录，实现声爆强度对流场守恒变量的变分结果向各个进程装配，将装配结果作为流场伴随方程的右端项实现流场声爆耦合伴随方程的求解。此外，对小型超声速公务机开展了声爆优化，对比分析了设计前后的声压及其频谱特性。     

一般均衡模型下的税负归宿研究

税负归宿问题因其复杂的传导机制影响着人们对最终税收负担的判断，在局部均衡分析失效的情况下，一般均衡模型是研究税负归宿的更佳方案。基于经典的Harberger模型，运用线性化和逼近技术，讨论了一般均衡框架下的数量求解算法，得到了特定部门资本和劳动用量以及资本价格的微分值，并以此分析了局部要素税的税负归宿以及最终的税收负担。     

天波超视距雷达的发展

 天波超视距雷达 (OTHR)是一种利用电离层对高频信号的反射作用自上而下进行目标探测的雷达体制。由于该雷达具有大范围的监视能力、防低空突袭、抗隐身以及早期预警等突出优点 ,受到了许多国家的重视。首先介绍了OTHR的性能特点及发展历史 ,接着就雷达的总体结构、干扰的抑制、由电离层引起的信号失真的校正 ,以及信号检测进行了全面的综述 ,最后指出这一领域今后的发展方向。     

飞机尾翼载荷飞行测量研究

 用分析和模型试验方法难以确定可靠的尾翼载荷,所以要求通过飞行试验获取尾翼载荷数据,但因测载技术复杂,精确地测定尾翼载荷亦是困难的。我们经过多年的工作,最终用应变法得到了可贵的某型飞机尾翼机动载荷测量结果。本文叙述了测量方法,并给出了垂尾载荷的部分测量结果。根据该结果对垂尾的受载情况提出了值得重视的看法。     

最大标准差和最大变异系数方法

本文提出的最大标准差方法和最大变异系数方法,能充分利用以往数据和经验提供的信息,大大减少了试件个数。与国际上常用的单侧容限系数法相比,可节省大量试件;而在试件个数相同的情况下,则可得到更接近母体百分位值的置信下限(如安全寿命或安全疲劳极限等)。