Features of whistling electromagnetic wave propagation descending from above upon the night ionosphere

The results of numerical solution of the wave equations for the oblique incidence of whistling electromagnetic waves upon the night ionosphere from above have been obtained and analyzed. In the studied region of altitudes, within the wavelength scale, charged particle concentration varies drastically, and damping caused by collisions between the charged and neutral particles decreases considerably. Below, the sharp lower boundary of the ionosphere, the refractive index of the whistler wave approaches unity, and plasma turbulence transform into atmospheric electromagnetic waves. The dependences of the whistler reflection factor are found in terms of energy and horizontal magnetic component of the electromagnetic wave near the Earth’s surface on the frequency and the wave vector transverse component for the plain-layered medium model at two values of latitude. Strong dependences have been found on the wave angle of incidence and frequency. At rather small angles of incidence, the wave disturbances reach the Earth’s surface, and the module of reflection coefficient logarithm is in the range of 0.4–1. At large angles of incidence, the reflection coefficient module varies over a wide range depending on specific conditions. The obtained results explain the absence of oscillation modes of plasma magnetosphere maser in the night magnetosphere.     

Design of Interplanetary Transfers with Passive Gravity Assists and Deep Space Maneuvers

In the paper, the problem of designing interplanetary trajectories with several swing-bys and deep-space maneuvers is solved using the method of virtual trajectories developed by the authors. The algorithms for the calculation of both heliocentric and planetocentric trajectory arcs are presented, including the case of resonant trajectories. The results of applying the method of virtual trajectories to the problem of designing an interplanetary transfer to Jupiter are given and compared with the baseline trajectories for the Juno, Europa Clipper, and Laplace missions.     

天地一体化信息网络空间激光通信新技术

空间激光通信是提升天地一体化信息网络传输速率、组网能力、信息安全的重要途径。结合天地一体化信息网络特点,总结国外空间激光通信技术的发展状况,分析有望应用于天地一体化信息网络中的空间激光通信新技术及其优势。希望通过借鉴国外空间激光通信技术发展的经验与启示,促进我国空间激光通信新技术的发展以及天地一体化网络的建设。     

用于痕量气体检测的宽调谐外腔量子级联激光器研究

研究基于闪耀光栅的Littrow外腔量子级联激光器,设计一种改进型Littrow外腔腔型,实现了小型化样机研制。测试结果表明,输出激光波长调谐范围1317cm^–1(7.593μm)至983cm^–1(10.173μm),最大平均功率17.7m W,激光线宽小于1cm^–1,功率稳定性优于0.5%(4h),波长稳定性优于0.12cm^–1(5.4h)。样机激光头尺寸76mm×54mm×50mm,部分技术指标优于国外商业产品。     

基于ICKF的永磁同步电机无传感器控制方法

针对在永磁同步电机(Permanent magnet synchronous motor,PMSM)中安装传感器带来的高成本、体积增大、可靠性降低和易受环境干扰等问题,提出采用迭代容积卡尔曼滤波(Iterative cubature Kalman filter,ICKF)算法来估计电机转速和转子位置,并将其应用于永磁同步电机无传感器控制。首先,建立了PMSM在α-β坐标系下的离散数学模型。其次,在Matlab/Simulink环境下分别建立了基于容积卡尔曼滤波(Cubature Kalman filter,CKF)和ICKF的PMSM转速、电流双闭环的无传感器矢量控制系统仿真模型,并进行了给定转速和加负载两种工况的仿真验证。最后,基于TMS320F28335芯片搭建了硬件实验验证平台。仿真分析与实验结果均表明,迭代容积卡尔曼滤波算法应用于永磁同步电机无传感器控制中抗负载变化干扰性好、电机运行稳定、电机转速和转子位置估计精度高,可满足对电机精确控制要求较高的应用场合,具有重要参考价值和推广意义。     

Steady, pseudo-steady and unsteady shock wave reflections

The reflection of oblique shock waves has been the subject of numerous experimental, analytical and numerical studies in the past five decades. In the past six years three reviews have been published on various aspects of shock wave phenomena by Griffith (1981), Bazhenova et al. (1984) and Hornung (1985). However, these reviews were not devoted completely to shock wave reflection phenomena and as such they are more limited in scope than the present review. Furthermore, the developments since these reviews were written suggested a need for an up-to-date comprehensive review. The present review is aimed at describing in detail the entire shock wave reflection phenomenon from a phenomenological point of view. It is divided into three parts. The first is dedicated to the reflection in pseudo-steady flows, e.g., shock tube experiments over straight wedges, the second concentrates on steady flows, e.g., wind tunnel experiments, and the third describes the phenomenon in truly unsteady flows, e.g., shock tube experiment over non-straight wedges, spherical blast wave reflections, etc. In each of these flow patterns, unsolved problems are discussed and future research needs are identified. In order to keep this review within an acceptable size it was decided not to include details of numerical studies. Whenever possible the nomenclature is the one suggested by Ben-Dor and Dewey (1985).     

Magnetospheric Science Objectives of the <Emphasis Type="Italic">Juno</Emphasis> Mission

In July 2016, NASA’s Juno mission becomes the first spacecraft to enter polar orbit of Jupiter and venture deep into unexplored polar territories of the magnetosphere. Focusing on these polar regions, we review current understanding of the structure and dynamics of the magnetosphere and summarize the outstanding issues. The Juno mission profile involves (a) a several-week approach from the dawn side of Jupiter’s magnetosphere, with an orbit-insertion maneuver on July 6, 2016; (b) a 107-day capture orbit, also on the dawn flank; and (c) a series of thirty 11-day science orbits with the spacecraft flying over Jupiter’s poles and ducking under the radiation belts. We show how Juno’s view of the magnetosphere evolves over the year of science orbits. The Juno spacecraft carries a range of instruments that take particles and fields measurements, remote sensing observations of auroral emissions at UV, visible, IR and radio wavelengths, and detect microwave emission from Jupiter’s radiation belts. We summarize how these Juno measurements address issues of auroral processes, microphysical plasma physics, ionosphere-magnetosphere and satellite-magnetosphere coupling, sources and sinks of plasma, the radiation belts, and the dynamics of the outer magnetosphere. To reach Jupiter, the Juno spacecraft passed close to the Earth on October 9, 2013, gaining the necessary energy to get to Jupiter. The Earth flyby provided an opportunity to test Juno’s instrumentation as well as take scientific data in the terrestrial magnetosphere, in conjunction with ground-based and Earth-orbiting assets.     

用于故障穿越的飞轮储能双三相异步电机驱动控制研究

随着海上风电场的发展和高压直流输电技术的应用,风电场系统存在交流侧故障穿越的问题。针对这个问题,提出了一种用于故障穿越的基于模块化多电平变频器和双三相异步电机的飞轮储能系统,并设计了其驱动控制方案。飞轮储能系统采用了模块化多电平技术能方便地构建大功率高压变频器,并具备扩容能力。为了提高飞轮储能系统的可靠性,采用了双三相异步电机驱动,从而提高了冗余性。接着设计了能均衡各个模块电容电压的双三相异步电机驱动控制算法。最后,基于MATLAB/Simulink仿真平台建立了风电场和飞轮储能系统的仿真模型,进行了仿真计算。仿真结果验证了飞轮储能系统的功能和驱动控制策略的性能。     

Observation of Terrestrial gamma-ray flashes in the RELEC space experiment on the <Emphasis Type="Italic">Vernov</Emphasis> satellite

The RELEС scientific payload of the Vernov satellite launched on July 8, 2014 includes the DRGE spectrometer of gamma-rays and electrons. This instrument comprises a set of scintillator phoswich-detectors, including four identical X-ray and gamma-ray detector with an energy range of 10 kev to 3 MeV with a total area of ~500 cm² directed to the atmosphere, as well as an electron spectrometer containing three mutually orthogonal detector units with a geometric factor of ~2 cm² sr. The aim of a space experiment with the DRGE instrument is the study of fast phenomena, in particular Terrestrial gamma-ray flashes (TGF) and magnetospheric electron precipitation. In this regard, the instrument provides the transmission of both monitoring data with a time resolution of 1 s, and data in the event-by-event mode, with a recording of the time of detection of each gamma quantum or electron to an accuracy of ~15 μs. This makes it possible to not only conduct a detailed analysis of the variability in the gamma-ray range, but also compare the time profiles with the results of measurements with other RELEC instruments (the detector of optical and ultraviolet flares, radio-frequency and low-frequency analyzers of electromagnetic field parameters), as well as with the data of ground-based facility for thunderstorm activity. This paper presents the first catalog of Terrestrial gamma-ray flashes. The criterion for selecting flashes required in order to detect no less than 5 hard quanta in 1 ms by at least two independent detectors. The TGFs included in the catalog have a typical duration of ~400 μs, during which 10–40 gamma-ray quanta were detected. The time profiles, spectral parameters, and geographic position, as well as a result of a comparison with the output data of other Vernov instruments, are presented for each of candidates. The candidate for Terrestrial gamma-ray flashes detected in the near-polar region over Antarctica is discussed.     

Designing corrections for the trajectory of the <Emphasis Type="Italic">Spektr-R</Emphasis> spacecraft in the event of immersions into the Moon’s sphere of influence

The results of updating the parameters of motion of the Spektr-R spacecraft at the end of 2016 have shown that, in January 2018, with a probability close to unity, the condition that a spacecraft stay in the Earth’s shadow is violated; however, in May of the same year, the ballistic life of the spacecraft will be terminated. Thus, in 2017, the question arose of how to design the correction of flight of this spacecraft using its onboard propulsion system. The correction was designed with allowance for the fact that, for the first time since it was launched, the spacecraft in the course of several years, beginning with 2017, repeatedly approaches the Moon, deeply immersing into its sphere of influence. This paper presents the technologically and organizationally convenient, allowable versions of upcoming correction of the Spektr-R spacecraft trajectory and justifies the particular scheme of its implementation.