一种改进的视线角加速度非线性估计与滤波方法研究

为消除采用跟踪-微分器渐进估计视线角加速度形成非线性比例微分(PD)型比例导引以提高末制导精度时因减小估计器产生的视线角加速度延迟形成的估计抖振噪声,提出了一种具有输出限幅的非线性跟踪-微分器和输出二阶低通滤波的视线角加速度估计滤波方案。仿真结果表明,该方案可明显减少估计抖振噪声和误差。滤波器参数对视线角加速度估计的消噪噪声和制导精度提高作用明显,一般宜采用低阻尼比的二阶低通滤波器。     

Alfvén waves as a driving mechanism in stellar winds

Alfvén waves have been invoked as an important mechanism of particle acceleration in stellar winds of cool stars. After their identification in the solar wind they started to be studied in winds of stars located in different regions of the HR diagram. We discuss here some characteristics of these waves and we present a direct application in the acceleration of late-type stellar winds.     

O5+ in High Speed Solar Wind Streams: SWICS/Ulysses Results

Recent observations with UVCS on SOHO of high outflow velocities of O⁵⁺ at low coronal heights have spurred much discussion about the dynamics of solar wind acceleration. On the other hand, O⁶⁺ is the most abundant oxygen charge state in the solar wind, but is not observed by UVCS or by SUMER because this helium-like ion has no emission lines falling in the wave lengths observable by these instruments. Therefore, there is considerable interest in observing O⁵⁺ in situ in order to understand the relative importance of O⁵⁺ with respect to the much more abundant O⁶⁺. High speed streams are the prime candidates for the search for O⁵⁺ because all elements exhibit lower freezing-in temperatures in high speed streams than in the slow solar wind. The Ulysses spacecraft was exposed to long time periods of high speed streams during its passage over the polar regions of the Sun. The Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses is capable of resolving this rare oxygen charge state. We present the first measurement of O⁵⁺ in the solar wind and compare these data with those of the more abundant oxygen species O⁶⁺ and O⁷⁺. We find that our observations of the oxygen charge states can be fitted with a single coronal electron temperature in the range of 1.0 to 1.2 MK assuming collisional ionization/recombination equilibrium with an ambient Maxwellian electron gas. This revised version was published online in June 2006 with corrections to the Cover Date.     

Modeling PSBL high speed ion beams observed by Cluster and Double Star

On October 8, 2004, the Cluster and Double Star spacecraft crossed the near-Earth (12–19 R_E) magnetotail neutral sheet during the recovery phase of a small, isolated substorm. Although they were separated in distance by ∼7 R_E and in time by ∼30 min, both Cluster and Double Star observed steady, but highly structured Earthward moving >1000 km/s high speed H⁺ beams in the PSBL. This paper utilizes a global magnetohydrodynamic (MHD) simulation driven by Wind spacecraft solar wind input to model the large-scale structure of the PSBL and large-scale kinetic (LSK) particle tracing calculations to investigate the similarities and differences in the properties of the observed beams. This study finds that the large-scale shape of the PSBL is determined by the MHD configuration. On smaller scales, the LSK calculations, in good qualitative agreement with both Cluster and Double Star observations, demonstrated that the PSBL is highly structured in both time and space, on time intervals of less than 2 min, and spatial distances of the order of 0.2–0.5 R_E. This picture of the PSBL is different from the ordered and structured region previously reported in observations.     

涡扇发动机装机状态自然低温试验

为完成涡扇发动机状态鉴定，在北方场站开展了发动机装机状态下的自然环境低温试验。通过地面试验完成了自然低 温试验环境的量化分析，研究了不同气源起动模式、不同使用方法对装机状态自然低温条件下发动机起动性能的影响，分析了发 动机样本量对试验鉴定结果的影响。结果表明：APU供气是低温冷浸透起动的首选起动方式；冷运转可以有效改善发动机低温起 动性能，使相对起动时间缩短0.125～0.250；增加发动机样本量可以获得更加科学的鉴定结果，在低温起动过程中，发动机可能出 现失速等不稳定现象，甚至造成起动失败。开展了飞行试验，研究了空中低温环境对发动机工作参数及加减速特性的影响。结果 表明：在相同高度和速度下发动机加速时间随进气温度的降低而延长，当空中进气温度相差约30 ℃时，加速时间延长最多约为 18%；减速时间随进气温度的变化不大。     

Furthering our understanding of electrostatic solitary waves through Cluster multispacecraft observations and theory

Nonlinear isolated electrostatic solitary waves (ESWs) are observed routinely at many of Earth’s major boundaries by the Wideband Data (WBD) plasma wave receivers that are mounted on the four Cluster satellites. The current study discusses two aspects of ESWs: their characteristics in the magnetosheath, and their propagation in the magnetosheath and in the auroral acceleration (upward current) region. The characteristics (amplitude and time duration) of ESWs detected in the magnetosheath are presented for one case in which special mutual impedance tests were conducted allowing for the determination of the density and temperature of the hot and cold electrons. These electron parameters, together with those from the ion experiment, were used as inputs to an electron acoustic soliton model as a consideration for the generation of the observed ESWs. The results from this model showed that negative potential ESWs of a few Debye lengths (10–50 m) could be generated in this plasma. Other models of ESW generation are discussed, including beam instabilities and spontaneous generation out of turbulence. The results of two types of ESW propagation (in situ and remote sensing) studies are also presented. The first involves the propagation of bipolar type ESWs from one Cluster spacecraft to another in the magnetosheath, thus obtaining the velocity and size of the solitary structures. The structures were found to be very flat, with large scale perpendicular to the magnetic field (>40 km) and small scale parallel to the field (<1 km). These results were then discussed in terms of various models which predict such flat structures to be generated. The second type of propagation study uses striated Auroral Kilometric Radiation (SAKR) bursts, observed on multiple Cluster satellites, as tracers of ion solitary waves in the upward current region. The results of all studies discussed here (pulse characteristics and ESW velocity, lifetime, and size) are compared to in situ measurements previously made on one spacecraft and to theoretical predictions for these quantities, where available. The primary conclusion drawn from the propagation studies is that the multiple spacecraft technique allows us to better assess the stability (lifetime) of ESWs, which can be as large as a few seconds, than can be achieved with single satellites.     

加速度作用下环路热管工作特性实验

针对单储液器环路热管在过载加速度作用下可能出现的温度波动甚至无法运行的问题,基于恒加速度离心机系统,建立了双储液器环路热管(DCCLHP)工作特性实验台,实验研究了双储液器环路热管在重力场稳定运行后再施加过载加速度时的工作特性,分析了不同加热功率、不同加速度大小和方向对其运行性能的影响.结果表明,双储液器环路热管在加速度为7g时仍可达到稳定工作状态,加速度作用导致其稳定运行温度低于地面重力场的温度,且随加热功率和加速度不同,运行温度降低程度不同;加速度方向沿储液器2指向储液器1时其达到稳定状态所需时间比其反方向时更短.实验还观察到了加速度作用下冷凝器出口和液体管线出口温度波动现象.      

激光加速电子研究进展及其在空间环境模拟中的应用前景

超短超强激光与等离子体相互作用可以产生极端的物态条件和电离辐射环境, 这为航天器空间环境模拟研究提供了条件。文章综述了激光加速电子技术的基本原理和近年来的研究进展, 介绍了包括空泡机制在内的几种重要的加速机制, 重点回顾了电子束的能量提升和束流品质改善两方面的理论和实验结果。此外, 对激光电子加速应用于未来航天器空间环境模拟研究进行了展望。     

亚暴偶极化中近地磁尾质子的非绝热加速

亚暴偶极化过程中离子加速是亚暴粒子注入的重要产生机制. 通过试验粒子的方法模拟研究了亚暴偶极化期间磁尾等离子体片-8R_e～-5R_e处超低频电磁波对质子的加速过程. 研究表明, 质子在大尺度偶极化电磁场的作用下向内磁层注入, 与质子回旋频率相近的超低频电磁波能够引起低能质子发生非绝热加速. 质子在偶极化前后的能量变化与质子的初始能量密切相关, 初始能量远小于截止能量的质子, 末能量要比初始能量显著增加, 其值与扰动波频率相关, 且量级与偶极化造成的低能氧离子能量增加量级基本相当; 初始能量在截止能量以上的质子受超低频电磁波影响不大, 注入过程能量基本保持不变.      

Zero,minimum and maximum relative radial acceleration for planar formation flight dynamics near triangular libration points in the Earth–Moon system

Assume a constellation of satellites is flying near a given nominal trajectory around _L4$L_4$ or _L5$L_5$ in the Earth–Moon system in such a way that there is some freedom in the selection of the geometry of the constellation. We are interested in avoiding large variations of the mutual distances between spacecraft. In this case, the existence of regions of zero and minimum relative radial acceleration with respect to the nominal trajectory will prevent from the expansion or contraction of the constellation. In the other case, the existence of regions of maximum relative radial acceleration with respect to the nominal trajectory will produce a larger expansion and contraction of the constellation. The goal of this paper is to study these regions in the scenario of the Circular Restricted Three Body Problem by means of a linearization of the equations of motion relative to the periodic orbits around _L4$L_4$ or _L5$L_5$. This study corresponds to a preliminar planar formation flight dynamics about triangular libration points in the Earth–Moon system. Additionally, the cost estimate to maintain the constellation in the regions of zero and minimum relative radial acceleration or keeping a rigid configuration is computed with the use of the residual acceleration concept. At the end, the results are compared with the dynamical behavior of the deviation of the constellation from a periodic orbit.