The Physical Foundation of Forecasting Disturbances in the Geospace From Solar Disk Characteristics

The five main types of antisunward propagating energetic fluxes (particles and emission) may be thought of as well established to date, the effects of which lead to a particilar character of disturbance in the near-terrestrial environment (the Earth's magnetosphere, ionosphere and atmosphere). The strongest global restructuring of the magnetosphere and ionosphere is caused by fluxes of relatively dense n of 1-70 cm-3 at the Earth's orbit) Solar Wind (SW) quasi-neutral, low-energy (E ＜ 10 keV) plasma which cause magnetospheric and ionospheric storms lasting 24 hours or longer. For that reason, main attention is given to their study at the initial stage of research. The physical essence of the method of predicting disturbances in the near-terrestrial space environment, the amplitude of which can be expressed in, for example, the Kp index units, involves:(1) identifying all the most geo-effective SW streams of type, (2) determing their sources on the solar disk,and (3) quantifying the correlations between the characteristics of their solar sources with a maximum value of the Kp-index that is caused by the concerned type of SW stream. Semi-phenomenological relations have been obtained, which relate parameters of type SW stream sources to characteristics of geomagnetic storms:storm commencement, the time at which the storm intensity reaches its maximum values, the storm duration,as well as to the storm amplitude expressed in terms of geomagnetic indeces.      

Study of the Enhancement Events of Relativistic Electron at the Geosynchronous Orbit

The high flux of energetic electron on geostationary orbit can induce many kinds of malfunction of the satellite there, within which the bulk-charging is the most significant that several broadcast satellite failures were confirmed to be due to this effect. The electron flux on geostationary orbit varies in a large range even up to three orders accompanied the passage of interplanetary magnetic cloud and the following geomagnetic disturbances. Upon the investigation of electron flux enhancement events, two types of events were partitioned as recurrent events and random ones. Both of the two kinds of events relate to the interplanetary conditions such as solar wind parameters, IMF etc and their evolution characters as well. As for the recurrent events, we found that, (1) all of the events exhibits periodic recurrence about 27 days, (2) significant increase of electron flux relates to interplanetary index and characters of their distribution, (3) the electron flux also has relation to solar activity index. An artificial neural network was constructed to estimate the flux I day ahead. The random electron flux enhancement events are rare and present different distribution figures to the recurrent ones. The figure of the random events and the conditions of their occurrence is also discussed in this paper.      

转动帆板红外热流计算及等效方法研究

目前的空间外热流分析软件和在航天器稳态热平衡试验中模拟的外热流都不包括帆板对航天器表面的红外加热,而有时帆板的红外加热并不小,应该叠加到模拟的外热流中.文章针对一种低轨道航天器,计算了帆板红外加热的强度,给出了在热平衡试验中叠加的方法,并讨论了在固定帆板方位的同时保持其红外热流等效的可能性.结果表明,可以精确计算帆板红外加热,对任意的帆板方位均可以保持其红外加热的等效.     

第2009卡林顿周太阳活动的初步分析

介绍了第 2 0 0 9卡林顿周大黑子群AR484,AR486和AR488产生的太阳活动以及这些太阳活动对地球空间环境造成的影响。依据对太阳活动的统计研究 ,简要分析了三个大黑子群活动的差异。分析结果指出 ,关注某一时期太阳活动的活动经度带以及太阳活动在某一半球的主次是解决太阳活动短期预报非常重要的思路     

卫星太阳电池阵在板展开阶段的撞击特性研究

研究了卫星太阳电池阵在板展开阶段的撞击特性,导童重要性一多体系统的动力学方程,介绍了撞击力的计算方法,计算了太阳电池阵在撞击阶段的撞击力和一些特殊节点的加速度和变化规律,计算结果表明,各点的撞击力在不同的时刻达到峰值,说明柔性板在撞击时发生了扭转,此外还发现靠近撞击处的节点的加速度在撞击瞬间比其它节点大,通过冲击波的传播引起外侧板的边界上节点的加速度不断上下振动,可以解释外侧帆板在撞击后上下、左右     

基于隶属度和LMK-ELM的航空电子部件诊断方法

为提高航空电子部件模块级故障诊断精度，提出一种新的面向"软聚类"的局部多核学习（LMKL）-超限学习机（ELM）离线诊断方法。通过引入模糊C均值聚类对样本空间进行模糊划分，挖掘聚类内部多样性的同时，实现了对过学习的抑制；将模糊划分产生的隶属度信息融入LMKL-ELM的优化过程，运用基于初始-对偶混合优化问题的三步优化策略克服了局部核权重二次非凸的问题，在l₁-范数与l₂-范数约束下分别给出了相应的更新方法。将所提方法应用于某型机前端接收机，结果表明：与4种流行的多核诊断方法相比，该方法可有效避免漏警、抑制虚警，在l₁-范数和l₂-范数约束下，其诊断精度比其他方法的平均值分别提升了4.09%和5.13%。     

极端低温下电液伺服阀温漂特性分析

针对电液伺服阀在极端低温下温漂大的问题，以＋40℃时电液伺服阀初始零偏为基准，采用线性回归方法分析了某型射流管伺服阀不同温度的零偏试验数据，得到了极端低温下的伺服阀温漂与＋40℃时初始零偏的数学关系。分析与试验结果表明：极端低温时射流管伺服阀的温漂与＋40℃时的初始零偏存在非常显著的线性关系。温漂与电液伺服阀制造与装配工艺过程密切相关，与结构及其装配不对称有关。电液伺服阀结构上的微观不对称现象，在极端低温下显现出来，尤其是呈现出较大的温漂。降低温漂的主要措施是提高电液伺服阀结构与装配的对称性，降低初始零偏。     

玫瑰扫描光学系统头罩气动热建模与仿真

在导弹高速飞行过程中，光学头罩的温度受气动热效应作用而急剧升高，会产生严重的气动热辐射效应。为研究头罩气动热对玫瑰扫描光学系统的影响，建立了基于CFD流体仿真软件的头罩温度场模型。在仿真软件对光学系统结构进行三维建模后，通过光学软件对头罩热辐射对探测器的影响进行了仿真和计算。仿真结果表明：玫瑰扫描光学系统对头罩的温度梯度较为敏感，当头罩温度非均匀分布时，探测器会接收到气动热辐射干扰信号，对弱小目标的正常探测和提取产生干扰，气动热辐射效应不容忽视。     

Multi-wavelength coordinated observations of ionospheric irregularity structures from an anomaly crest location during unusual solar minimum of the 24th cycle

The present paper reports coordinated ionospheric irregularity measurements at optical as well as GPS wavelengths. Optical measurements were obtained from Tiny Ionospheric Photometer (TIP) sensors installed onboard the Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) satellites. GPS radio signals were obtained from a dual frequency GPS receiver operational at Calcutta (22.58°N, 88.38°E geographic; geomagnetic dip: 32.96°; 13.00°N, 161.63°E geomagnetic) under the SCIntillation Network Decision Aid (SCINDA) program. Calcutta is located near the northern crest of Equatorial Ionization Anomaly (EIA) in the Indian longitude sector. The observations were conducted during the unusually low and prolonged solar minima period of 2008–2010. During this period, four cases of post-sunset GPS scintillation were observed from Calcutta. Among those cases, simultaneous fluctuations in GPS Carrier-to-Noise ratios (C/N_o) and measured radiances from TIP over a common ionospheric volume were observed only on February 2, 2008 and September 25, 2008. Fluctuations observed in measured radiances (maximum 0.95 Rayleigh) from TIP due to ionospheric irregularities were found to correspond well with C/N₀ fluctuations on the GPS links observed from Calcutta, such effects being noted even during late evening hours of 21:00–22:00 LT from locations around 40° magnetic dip. These measurements indicate the existence of electron density irregularities of scale sizes varying over several decades from 135.6 nm to 300–400 m well beyond the northern crest of the EIA in the Indian longitude sector during late evening hours even in the unusually low solar activity conditions.