Magnetospheric and ionospheric manifestations of interplanetary foreshocks

The geometry of a typical interplanetary shock front in the vicinity of the Earth’s orbit predicts that the leading edge of the foreshock region comes into contact with the magnetosphere a few hours ahead of geomagnetic sudden impulses (SI). There is reason to believe that the interaction of the magnetosphere with the foreshock leads to magnetic and ionospheric disturbances, which can be detected by ground-based instruments. We searched for specific precursors of SIs in data from the Scandinavian riometer network and in the short period geomagnetic pulsation data from mid-latitude magnetometers. We found that SIs were preceded by the following three features: (1) an increase in riometric absorption, (2) excitation of Pcl magnetic pulsations and (3) a spectral broadening of the Pc3 magnetic pulsations. Our observations may be useful for the study of acceleration processes in the solar wind. These observations are also of potential forecasting interest.     

Dissipative Solitary Kinetic Alfvén Waves and Electron Acceleration in the Solar Corona

Nonthermal electrons play a major role during solar flares since not only they contain a large amount of the released energy but also they provide important information of the flaring physics through their nonthermal radiation in radio and hard X-ray bands. In a recent work Wu (Phys. Plasmas 10 (2003) 1364) proposed that dissipative solitary kinetic Alfvén wave (DSKAW) with a local shock-like structure could provide an efficient acceleration mechanism for energetic electrons in a low-β plasma. In the present paper dynamical characteristics of the DSKAW acceleration mechanism in solar coronal plasmas are studied and its application to the acceleration of flaring electrons is discussed.     

圆锥激波的反解法

给出了超音速圆锥激波的一种反解法，该方法由假定的激波处向锥面推算，具有计算效率高，适于计算机处理等特点。     

子午面内Alfvén波的传播特征

本文使用由ＷＫＢ近似得到的Ａｌｆｖｅｎ波传播的张量表达式,具体计算和讨论了一种太阳子午面内含盔形－电流片磁位形的流场中Ａｌｆｖｅｎ波的传播特征,主要结果是：（１）Ａｌｆｖｅｎ波磁场起伏随日心距离的增加而衰减,其中极开区的衰减远快于赤道区,但随着距离的增大,这种纬度关系将迅速变弱,以致在较远空间,磁起伏相差很小,衰减很慢;（２）Ａｌｆｖｅｎ波的相对磁场起伏ｂ／Ｂ随着距离的增加而迅速增大,在几个太阳半径之后变化不再明显,达到所谓的＂饱和＂;在大日心距离的盔形电流片附近,Ａｌｆｖｅｎ波将成为重要的磁场组成部分;（３）Ａｌｆｖｅｎ波速度起伏纬度关系较为明显,相对速度起伏。ｕ／Ｕ随着距离增大而衰减,电流片区衰减得较快,但这种纬度差别将变弱．与黄道面内Ａｌｆｖｅｎ波传播特征的具体比较表明,磁场涨落的变化特征与背景场位形存在着十分密切的关系,但速度涨落与背景场没有这种明显关系．     

电磁场对航空电子设备干扰的预测研究

论述飞机内部辐射电磁通过电缆线感应耦合，形成对电子设备干扰的机理，分析这种干扰模式既有辐射，又有传导的复合特点。应用孔缝衍射、场对线激励、含分布源传输线和网络分析等理论与方法，逐层剖析描述了预测数学模型，并给出了能够对电子设备电子元件级进行可靠性和安全性评估的实用预测软件。     

紧缩平面场扫描架系统研制

紧缩平面场(CATR)是在较小的微波暗室里模拟远场的电磁环境,以行进各种天线的测量和研究.其最终性能指标要由紧缩平面场扫描架评定.根据紧缩平面场扫描测量原理,及其对扫描架平面度、直线度、定位精度及自动化程度的要求,研制了极坐标型紧缩场扫描架系统,通过采用高精度直线导轨、平面度微调方式和基于工业控制计算机的数字控制技术,达到了所要求的检测精度,满足了紧缩平面场扫描测量的要求.     

直升机机内PWM照明调光系统产生音频干扰问题的研究

在直升机机内照明调光领域，国外军机已广泛采用脉冲宽度调制（PWM）调光方式。PWM调光方式相比传统线性调光方式具有以下明显优点：效率高，调光范围宽，功耗小，带载能力强，附加损耗小等。但PWM调光系统的不足是电磁辐射，尤其会对机内通话系统产生音频干扰，在机通耳机中会出现明显干扰声，影响机内通话质量。本方案能有效抑制PWM...     

Tearing,coalescence and fragmentation processes in solar flare current sheet and drifting pulsating structures

The paper presents a summary of results from two different simulations which study the tearing, coalescence and fragmentation of current sheets, the associated production of energetic electrons and of plasma waves from these electrons which could explain drifting pulsation structures observed at radio wavelengths. Using a 2.5-D particle-in-cell (PIC) model of the current sheet it is shown that due to the tearing mode instability the current sheet tears into plasmoids and these plasmoids later on coalesce into larger ones. During these processes electrons are accelerated and they produce observable electromagnetic waves. Furthermore, the 3-D PIC model with two current sheets extended in the electric current direction shows their fast fragmentation associated with the exponential dissipation of the free magnetic field energy. An example of the drifting pulsating structure which is considered to be a radio signature of the above mentioned processes in solar flares is shown.     

Simultaneous observations of some unusual whistlers and VLF hiss emission at a low L-value (L = 1.17)

The purpose of this paper is to describe some unusual whistlers (doublets and triplets) and VLF hiss emission recorded simultaneously on February 18, 1998 during nighttime at a low latitude Indian ground station Jammu (geomag. lat., 22° 26′ N; L = 1.17), and to make some discussions about their origin. The detailed structures of the observed VLF hiss emission clearly show that these emissions confined to a narrow continuous frequency band. Some times the frequency of hiss band oscillates and subsequently touches the upper edge of the first whistler component of the doublet. Detailed structures of the dynamic spectra of whistler and VLF hiss emission are briefly presented. From the dispersion analysis of the whistler doublets and triplets, it is found that the individual whistlers of the doublets and triplets simultaneously observed on the same day are one-hop whistlers having propagation path along higher and closely spaced L-values. Our result also shows that VLF hiss has been generated in the equatorial region of higher L-values. Generation and propagation mechanisms are briefly discussed.     

3D Imaging of the OH mesospheric emissive layer

A new and original stereo imaging method is introduced to measure the altitude of the OH nightglow layer and provide a 3D perspective map of the altitude of the layer centroid. Near-IR photographs of the OH layer are taken at two sites separated by a 645 km distance. Each photograph is processed in order to provide a satellite view of the layer. When superposed, the two views present a common diamond-shaped area. Pairs of matched points that correspond to a physical emissive point in the common area are identified in calculating a normalized cross-correlation coefficient (NCC). This method is suitable for obtaining 3D representations in the case of low-contrast objects. An observational campaign was conducted in July 2006 in Peru. The images were taken simultaneously at Cerro Cosmos (12°09′08.2″ S, 75°33′49.3″ W, altitude 4630 m) close to Huancayo and Cerro Verde Tellolo (16°33′17.6″ S, 71°39′59.4″ W, altitude 2272 m) close to Arequipa. 3D maps of the layer surface were retrieved and compared with pseudo-relief intensity maps of the same region. The mean altitude of the emission barycenter is located at 86.3 km on July 26. Comparable relief wavy features appear in the 3D and intensity maps. It is shown that the vertical amplitude of the wave system varies as exp (Δz/2H) within the altitude range Δz = 83.5–88.0 km, H being the scale height. The oscillatory kinetic energy at the altitude of the OH layer is comprised between 3 × 10⁻⁴ and 5.4 × 10⁻⁴ J/m³, which is 2–3 times smaller than the values derived from partial radio wave at 52°N latitude.