Ionospheric electron density over Resolute Bay according to E-CHAIM model and RISR radar measurements

In this study, predictions of the E-CHAIM ionospheric model are compared with measurements by the incoherent scatter radars RISR at Resolute Bay, Canada, in the northern polar cap. Reasonable coverage was available for all seasons except winter for which no conclusions were drawn. It is shown that ratios of the model-to measured electron densities are close to unity in the central part of the F layer, around its peak. This is particularly evident for summer daytime. Distributions of the ratios are wider for other seasons indicating larger number of cases when the model underestimates or overestimates. E-CHAIM underestimates the electron density at ionospheric topside and bottomside by ～ 10–20 %. At the bottomside, the underestimations are strongest in summer and equinoctial nighttime. At the topside, the underestimations are strongest in autumn nighttime. Model overestimations are noticeable in the middle part of the F layer during dawn hours in autumn. Overall, the model tends to not predict highest-observed peak electron densities and the largest-observed heights of the peak.     

Testing the three-dimensional IRI-SIRMUP-P mapping of the ionosphere for disturbed periods

This paper describes the three-dimensional (3-D) electron density mapping of the ionosphere given as output by the assimilative IRI-SIRMUP-P (ISP) model for three different geomagnetic storms. Results of the 3-D model are shown by comparing the electron density profiles given by the model with the ones measured at two testing ionospheric stations: Roquetes (40.8°N, 0.5°E), Spain, and San Vito (40.6°N, 17.8°E), Italy. The reference ionospheric stations from which the autoscaled foF2 and M(3000)F2 data as well as the real-time vertical electron density profiles are assimilated by the ISP model are those of El Arenosillo (37.1°N, 353.3°E), Spain, Rome (41.8°N, 12.5°E), and Gibilmanna (37.9°N, 14.0°E), Italy. Overall, the representation of the ionosphere made by the ISP model is better than the climatological representation made by only the IRI-URSI and the IRI-CCIR models. However, there are few cases for which the assimilation of the autoscaled data from the reference stations causes either a strong underestimation or a strong overestimation of the real conditions of the ionosphere, which is in these cases better represented by only the IRI-URSI model. This ISP misrepresentation is mainly due to the fact that the reference ionospheric stations covering the region mapped by the model turn out to be few, especially for disturbed periods when the ionosphere is very variable both in time and in space and hence a larger number of stations would be required. The inclusion of new additional reference ionospheric stations could surely smooth out this concern.     

电弧加热发动机羽流电子温度及电子数密度的双静电探针测量

研制了一套双静电探针测量系统,对以氩气为推进剂的1kW级电弧加热发动机羽流进行了测量,得到了电子温度和电子数密度的轴向和径向分布,以及随弧电流、气流量的变化趋势。结果表明,羽流显著偏离局域热力学平衡状态,电子温度呈现复杂的分布和变化趋势。羽流轴线上的电子温度明显低于偏离轴线处的值,而电子数密度远高于偏离轴线处的值;羽流轴线上的电子温度随弧电流的增加而降低,电子数密度随弧电流的增加而增加;羽流中心区电子温度随气流量的变化趋势不明显。     

TC11电子束焊接接头组织分析

以20mm厚TC11电子束焊接试样为研究对象,进行金相分析和显微硬度测试。对20mm板厚TC11钛合金电子束焊接接头组织及显微硬度进行了分析研究。比较分析了接头的焊缝、热影响区及各过渡界面的组织状态,并对不同组织的形成机理进行了阐释。     

基于网络计划技术的冷校靶流程

为提高飞机大修效率,缩短大修时间,对其中航炮冷校靶流程进行了分析,运用网络计划技术原理并根据逻辑关系绘制了航炮冷校靶网络图,采用关键线路法对关键工序进行优化,调整关键线路进而有效缩短航炮冷校靶时间,对于飞机大修其他工作流程也可应用网络计划技术,从而能有效地提高飞机大修效率。     

Pre-storm behaviour of NmF2 and TEC (GPS) over equatorial and low latitude stations in the Indian sector

The pre-storm behavior of NmF₂ and TEC over an equatorial station, Trivandrum (8.47°N, 76.91°E, dip 0.6°S) and a low latitude station, Waltair (17.7°N,83.3°E, dip 20°N) has been studied for a total of 18 strong geomagnetic storms with DST ? −100 nT. The simultaneous measurements of GPS-TEC and NmF₂ over Trivandrum and Waltair during the period 2000–2005 have been considered for the present study. It is found that there is a substantial increase in NmF₂ and TEC before the onset of the storm over Waltair, while the increase is not present at Trivandrum. The origin of pre-storm enhancements in electron density still remains unresolved owing to several conditions in their potential sources and occurrence mechanisms. In the present study an attempt is made to identify the possible mechanisms responsible for such enhancements in electron density of the F-region.     

电子回旋共振推力器放电室内磁场与微波电磁场分析

电子回旋共振推力器具有寿命长、比冲高、结构简单等特点,适宜用作深空探测器主推进装置。放电室是电子回旋共振推力器的关键部件,其作用是产生电子回旋共振等离子体。放电室内的磁场和微波电磁场分布对于推力器的可靠启动、稳定工作有着重要的影响。为此针对10cm推力器,采用大型有限元分析软件ANSYS建立了三种磁路模型,计算了放电室内的磁场分布,得出三种方案中电子回旋共振面的位置,分析放电室材料不同时磁场分布的变化;最后采用ANSYS有限元分析软件计算了放电室内的电磁场分布。结果表明,在电子回旋共振面上微波能量满足放电所需能量。计算结果可以为电子回旋共振推力器放电室的设计提供帮助。     

CAST空间碎片超高速撞击试验研究进展

超高速撞击试验是开展载人航天器及大型应用卫星空间碎片超高速撞击风险评估和防护设计的基础,作为我国航天器环境效应和可靠性工程验证部门的北京卫星环境工程研究所在这个领域做了大量的工作。文章介绍了二级轻气炮超高速撞击地面模拟试验技术、典型防护结构防护性能的超高速撞击试验验证、载人航天器外露材料超高速撞击特性、毫米级弹丸7 km/s以上超高速稳定发射技术探索、高性能防护结构研究等方面的若干近期进展。展望了我国空间碎片防护需求和地面超高速撞击试验研究的发展方向。     

日照边缘区域电离层对耀斑的响应特点研究

利用MSIS模型和背景太阳辐射谱模型,在一定大耀斑辐射谱假设的前提下,计算了耀斑期间日照边缘区域的电子产生率,分析了这一区域电离层电子密度的变化特点.结果表明,大耀斑期间在日照边缘区域,甚至大于太阳天顶角90°的区域都有明显的电子产生率的增加.从不同太阳天顶角处的电子产生率剖面的形态来看,随着天顶角的增加最大电离率减少,但高度增加.计算还显示了在太阳天顶角小于90°的区域内电子产生率的垂直分布有明显的双峰结构,这种结构对应着电离层的E区和F区,但在天顶角大于90°区域,F区的电子产生率要大得多.考虑到离子和电子的复合过程,这一区域的总电子含量的增加主要产生在高F区.      

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.