On halo orbits spacecraft stabilization

The paper deals with the application of recent non-linear control techniques to the problem of tracking and maintaining a given satellite on prescribed orbits around the so-called translunar libration point L₂. Such orbits, known in literature as Halo Orbits, have the property of ensuring visibility both from the dark side of the Moon and from Earth at any time. Their importance is strictly related to the placement of a base situated on the dark side of the Moon for advanced space missions as deep space observation, solar system exploration and scientific researches in a low gravity enviroment.

Because of the instability of the equilibrium L₂, such orbits cannot be maintained without an active control. In this paper we investigate the application of nonlinear control techniques to solve the problem. A comparison between linear and nonlinear methods is developed and simulation results are discussed.     

某型航空发动机进气压力畸变试验研究

针对飞机在大攻角飞行时易引起进气道和发动机进口流场畸变的情况,对某型发动机的综合抗进气压力畸变能力进行了整机试验研究。试验采用插板式畸变模拟器研究发动机综合抗总压畸变能力,获得了各规定风扇换算转速下发动机临界畸变指数,完成了畸变条件下遭遇加速试验,发动机过渡态工作正常。结果表明:该试验方案可行、数据可靠、结果有效,该型发动机满足飞机/发动机相容性试验要求。     

基于触发角定时控制的异步电机软起动控制器设计

针对起重设备专用三相异步电机的直接起动问题,分析了异步电机的T型等效电路,阐述了晶闸管调压电路的工作原理,提出了一种基于触发角定时控制的异步电机软起动方法。基于MATLAB/Simulink搭建了相应的系统仿真模型,进行了提出方法的仿真分析,验证了所提方法的正确性。最后,基于单片机设计了相应的软起动器的软硬件,进行了试验测试。结果表明提出的方法可以有效地实现三相异步电机的平滑起动,起动电流较小,有效地减少了起动过程对电机和电网的影响。     

Venus Atmospheric Thermal Structure and Radiative Balance

From the discovery that Venus has an atmosphere during the 1761 transit by M. Lomonosov to the current exploration of the planet by the Akatsuki orbiter, we continue to learn about the planet’s extreme climate and weather. This chapter attempts to provide a comprehensive but by no means exhaustive review of the results of the atmospheric thermal structure and radiative balance since the earlier works published in Venus and Venus II books from recent spacecraft and Earth based investigations and summarizes the gaps in our current knowledge. There have been no in-situ measurements of the deep Venus atmosphere since the flights of the two VeGa balloons and landers in 1985 (Sagdeev et al., Science 231:1411–1414, 1986). Thus, most of the new information about the atmospheric thermal structure has come from different remote sensing (Earth based and spacecraft) techniques using occultations (solar infrared, stellar ultraviolet and orbiter radio occultations), spectroscopy and microwave, short wave and thermal infrared emissions. The results are restricted to altitudes higher than about 40 km, except for one investigation of the near surface static stability inferred by Meadows and Crisp (J. Geophys. Res. 101:4595–4622, 1996) from 1 \(\upmu\)m observations from Earth. Little information about the lower atmospheric structure is possible below about 40 km altitude from radio occultations due to large bending angles. The gaps in our knowledge include spectral albedo variations over time, vertical variation of the bulk composition of the atmosphere (mean molecular weight), the identity, properties and abundances of absorbers of incident solar radiation in the clouds. The causes of opacity variations in the nightside cloud cover and vertical gradients in the deep atmosphere bulk composition and its impact on static stability are also in need of critical studies. The knowledge gaps and questions about Venus and its atmosphere provide the incentive for obtaining the necessary measurements to understand the planet, which can provide some clues to learn about terrestrial exoplanets.     

Water and Volatile Inventories of Mercury,Venus, the Moon,and Mars

We review the geochemical observations of water, \(\mbox{D}/\mbox{H}\) and volatile element abundances of the inner Solar System bodies, Mercury, Venus, the Moon, and Mars. We focus primarily on the inventories of water in these bodies, but also consider other volatiles when they can inform us about water. For Mercury, we have no data for internal water, but the reducing nature of the surface of Mercury would suggest that some hydrogen may be retained in its core. We evaluate the current knowledge and understanding of venusian water and volatiles and conclude that the venusian mantle was likely endowed with as much water as Earth of which it retains a small but non-negligible fraction. Estimates of the abundance of the Moon’s internal water vary from Earth-like to one to two orders of magnitude more depleted. Cl, K, and Zn isotope anomalies for lunar samples argue that the giant impact left a unique geochemical fingerprint on the Moon, but not the Earth. For Mars, an early magma ocean likely generated a thick crust; this combined with a lack of crustal recycling mechanisms would have led to early isolation of the Martian mantle from later delivery of water and volatiles from surface reservoirs or late accretion. The abundance estimates of Martian mantle water are similar to those of the terrestrial mantle, suggesting some similarities in the water and volatile inventories for the terrestrial planets and the Moon.     

Ion Composition of the Earth’s Radiation Belts in the Range from 100 keV to $100\mbox{ MeV}/\mbox{nucleon}$: Fifty Years of Research

Spatial, energy and angular distributions of ion fluxes in the Earth’s radiation belts (ERB) near the equatorial plane, at middle geomagnetic latitudes and at low altitudes are systematically reviewed herein. Distributions of all main ion components, from protons to Fe (including hydrogen and helium isotopes), and their variations under the action of solar and geomagnetic activity are considered. For ions with \(Z\geq 2\) and especially for ions with \(Z \geq 9\), these variations are much more than for protons, and these have no direct connection with the intensity of magnetic storms (\(Z\) is the charge of the atomic nucleus with respect to the charge of the proton). The main physical mechanisms for the generation of ion fluxes in the ERB and the losses of these ions are considered. Solar wind, Solar Cosmic Rays (SCR), Galactic Cosmic Rays (GCR), and Anomalous component of Cosmic Rays (ACR) as sources of ions in the ERB are considered.     

Daytime O/N<Subscript>2</Subscript> Retrieval Algorithm for the Ionospheric Connection Explorer (ICON)

The NASA Ionospheric Connection Explorer Far-Ultraviolet spectrometer, ICON FUV, will measure altitude profiles of the daytime far-ultraviolet (FUV) OI 135.6 nm and N₂ Lyman-Birge-Hopfield (LBH) band emissions that are used to determine thermospheric density profiles and state parameters related to thermospheric composition; specifically the thermospheric column O/N₂ ratio (symbolized as \(\Sigma\)O/N₂). This paper describes the algorithm concept that has been adapted and updated from one previously applied with success to limb data from the Global Ultraviolet Imager (GUVI) on the NASA Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) mission. We also describe the requirements that are imposed on the ICON FUV to measure \(\Sigma\)O/N₂ over any 500-km sample in daytime with a precision of better than 8.7%. We present results from orbit-simulation testing that demonstrates that the ICON FUV and our thermospheric composition retrieval algorithm can meet these requirements and provide the measurements necessary to address ICON science objectives.     

Pulsar Timing and Its Application for Navigation and Gravitational Wave Detection

Pulsars are natural cosmic clocks. On long timescales they rival the precision of terrestrial atomic clocks. Using a technique called pulsar timing, the exact measurement of pulse arrival times allows a number of applications, ranging from testing theories of gravity to detecting gravitational waves. Also an external reference system suitable for autonomous space navigation can be defined by pulsars, using them as natural navigation beacons, not unlike the use of GPS satellites for navigation on Earth. By comparing pulse arrival times measured on-board a spacecraft with predicted pulse arrivals at a reference location (e.g. the solar system barycenter), the spacecraft position can be determined autonomously and with high accuracy everywhere in the solar system and beyond. We describe the unique properties of pulsars that suggest that such a navigation system will certainly have its application in future astronautics. We also describe the on-going experiments to use the clock-like nature of pulsars to “construct” a galactic-sized gravitational wave detector for low-frequency (\(f_{GW}\sim 10^{-9} \text{--} 10^{-7}\) Hz) gravitational waves. We present the current status and provide an outlook for the future.     

电路测试响应信号的GP-KSVD稀疏重构算法

电路系统测试响应信号具有周期性强、分布较稀疏的特点,针对电路系统测试响应信号的压缩重构问题进行了研究,提出了基于梯度方向追踪的K奇异值分解(GPKSVD)稀疏重构算法。结合单一响应信号以及混合信号其自身特点进行字典训练,利用更新后字典对含噪信号进行梯度追踪稀疏表征,通过对含噪信号的重构,实现了去噪的目的,算法计算复杂度低,储存量小,具有较好的重构效果。仿真中将GP-KSVD表征与使用随机字典、离散余弦字典(DCT)的表征进行比较,从信噪比(SNR)以及相对均方误差(RMSE)2项指标中得出使用KSVD字典具有更好的重构去噪效果;此外将GP-KSVD稀疏重构算法与正交匹配追踪正交匹配追踪(OMP)-KSVD、预处理共轭梯度追踪(PCGP)算法进行比较,得出GP-KSVD的计算时间最短、重构精度更高的结论,并且进行了实测验证。算法可用来对测试响应信号进行预处理,为电路系统设备性能的评估分析提供了理论依据。     

航天用碳纳米管增强铝合金复合材料的力学与阻尼性能

碳纳米管(CNT)作为增强体的铝基复合材料(CNT/Al)具有轻质、高强、高模量、易加工的性能优势,用作轻量化材料在航天航空领域具有巨大的应用前景。为了获得兼顾其力学性能和阻尼性能的轻量化结构材料,采用叠片粉末冶金与合金化方法制备了质量分数为1.5% CNT/2A12复合材料,并研究了不同时效条件下的力学性能与阻尼性能。在130 ℃时效6~14 h时,复合材料具有最佳的拉伸强度与延伸率,抗拉强度最高可达595 MPa(时效12 h),延伸率最高可达14.0%(时效8 h)。复合材料的阻尼在0~180 ℃时变化不大,其在0.005左右,180~300 ℃时明显提高,300 ℃时可达0.05,阻尼性能受时效时间影响不大。复合材料的储存模量随测试温度升高而下降,在180~300 ℃时随振动频率升高而升高。时效条件为130 ℃-8 h时,质量分数1.5% CNT/2A12复合材料性能兼具良好的力学性能与阻尼性能。