直流稳压电源瞬态响应的测量

分析了直流稳压电源瞬态响应的技术要求 ,提出了电源瞬态响应的测量方法 。     

空间高能质子对航天器材料损伤的仿真分析

近地空间是各种载人飞船、应用卫星、空间站的主要活动区域,区域内存在大量由地磁场捕获的高能带电粒子,严重影响航天器和航天员的安全。为此,需要对内辐射带低高度空间的高能带电粒子环境及其通量分布进行研究。如何对质子进行有效屏蔽对空间辐射防护有重要的研究意义。文章针对粒子在空间环境中的辐射,简要介绍了质子在空间环境中的分布情况及在物质中的传输问题。利用SRIM软件模拟质子在不同材料(铝、聚乙烯)中输运过程。根据得到的射程与能量关系及对阻止本领的分析,从理论上提出航天器防护的合理方案。     

空间堆核动力技术选择研究

目前,基于太阳能、化学能的空间电源与空间推进技术,其技术能力的发展已接近极限状态,未来亟需开发基于核能的先进空间动力技术。针对低成本空间轨道运输、高功率载荷航天器、深空探测器、行星表面探测与开发等应用场景,以空间堆核电源为重点,分析了国际发展现状和未来航天需求,分别针对大功率(100 kWe～1 MWe)和小功率(1 kWe～10 kWe)应用需求,提出了技术主导方案,围绕主导技术方案梳理了关键技术,为我国空间堆核动力技术发展规划和预先研究提供参考。     

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.     

Solar flares,CMEs and solar energetic particle events during solar cycle 24

We present here a study of Solar Energetic Particle Events (SEPs) associated with solar flares during 2010–2014 in solar cycle 24. We have selected the flare events (≥GOES M-class), which produced SEPs. The SEPs are classified into three categories i.e. weak (proton intensity?≤?1?pfu), minor (1?pfu?<?proton intensity?<?10?pfu) and major (proton intensity?≥?10?pfu). We used the GOES data for the SEP events which have intensity greater than one pfu and SOHO/ERNE data for the SEP event less than one pfu intensity. In addition to the flare and SEP properties, we have also discussed different properties of associated CMEs.     

Classification of solar wind structures and intense geomagnetic storm alarms with self-organizing maps

Intense geomagnetic storms (D_st < −100 nT) usually occur when a large interplanetary duskward-electric field (with Ey > 5 mV m⁻¹) lasts for more than 3 h. In this article, a self-organizing map (SOM) neural network is used to recognize different patterns in the temporal variation of hourly averaged Ey data and to predict intense storms. The input parameters of SOM are the hourly averaged Ey data over 3 h. The output layer of the SOM has a total of 400 neurons. The hourly Ey data are calculated from solar wind data, which are provided by NSSDC OMNIWeb and ACE spacecraft and contain information on 143 intense storms and a fair number of moderate storms, weak storms and quiet periods between September 3, 1966 and June 30, 2002. Our results show that SOM is able to classify solar wind structures and therefore to give timely intense storm alarms. In our SOM, 21 neurons out of 400 are identified to be closely associated with the intense storms and they successfully predict 134 intense storms out of the 143 ones selected. In particular, there are 14 neurons for which, if one or more of them are present, the occurrence probability of intense storms is about 90%. In addition, several of these 14 neurons can predict big magnetic storm (D_st  −180 nT). In summary, our method achieves high accuracy in predicting intense geomagnetic storms and could be applied in space environment prediction.     

三维非线性撕裂模耦合和快速磁场重联

基于三维不可压缩电阻性ＭＨＤ方程，在长柱形位型下，数值研究了电阻撕裂模不稳定性所引起的磁场重联过程。研究结果表明，撕裂模的非线性相互作用和耦合，将产生许多模式的强裂解稳和导致快速的磁场重联。这一过程的进一步发展，导致具有螺旋形结构，不同模式的磁岛磁力线重叠，从而引起较大区域内的磁场各态经历和磁力线随机走向，形成撕裂模端动。     

Structure and development of quiet loops in the solar corona

X-ray emission from solar coronal loops changes on two different timescales: a) flare loops and transient active region brightenings show a rapid variability, b) quiet region loops are quasi-steady and change only slowly with time. This different time behavior has been analyzed on the basis of Yohkoh SXT observations and we report here on the results from our analysis, mainly focussing on quiet loop variability.     

应用微机校定三相变压器的联结组及标号

三相变压的联结组标号对其正常运行极为重要，必须校定，而目前变还缺少全面快捷的校定方法和设备。本文介绍采用微机系统来实现联结组桔的校定，首先把四类联结组差别区分开，然后分析指出同一类联结组中，除有六种正序标号外，存在六种逆序标号，提出用新的筛选法能简捷地判别校定同一类的十二种标号，当微机系统进行实际测试时，必须考虑电源电压三相不对称程序的影响，故经数学推导得出用实测计算值代替理想计算值作判别比较的基