EVA的形状记忆功能探讨

首先对形状记忆功能高分子的特性进行了分析,提出了形状记忆性能的评价指标,即形状回复率、形状固定率、形状回复速度等.并进一步探讨了乙烯-醋酸乙烯基共聚物(EVA)的形状记忆功能特性,研究发现,用过氧化二异丙苯(DCP)可对EVA进行适度交联,控制二者组分结构,从而控制EVA的交联程度,可使EVA具有优异的记忆功能特性,如形状回复率和形状固定率均可达95%以上;进一步分析了EVA的化学结构,讨论了分子结构与形状记忆性能的影响,并结合DMTA等热分析技术,对交联EVA的交联密度进行计算,结果表明EVA的交联点间分子量随DCP用量增加而下降,并且其交联程度与EVA的记忆特性存在着某种内在的必然联系,进一步研究分析发现其形状固定性与室温和橡胶态模量的比值呈线性关系,初步揭示了形状记忆机理.     

IXRF法用于航空发动机磨损在线监测的研究

 介绍了一种基于同位素X射线荧光法(IXRF法)的航空发动机磨损在线监测系统.航空发动机滑油中携带了大量的金属磨损屑末,利用不同金属释放出不同特征X射线的原理,可以检测出滑油中不同种类金属的成份及含量.此种方法具有快速、可靠、非接触等特点.实验结果表明,在线监测系统能够实时地检测出滑油中的铜、铁浓度.该项技术的研究和应用,可以对发动机的磨损故障进行早期预报,避免恶性事故的发生.     

火星磁场产生的原因及其分布

构建了一个可以得到火星赤道面上磁场分布的模型. 模型根据卫星观测数据, 提出了火星电离层、磁层顶和磁尾电流片上都各自通有电流的假设. 由电流的连续性条件可知, 这三种背景条件下的电流之间满足一定关系, 即火星磁层顶上的总电流是电离层上的总电流与磁尾电流片上的总电流之和. 这些电流产生的磁场与太阳风磁场共同构成了火星赤道面上磁场分布. 通过计算发现, 采用这种磁场模型得到的结果与目前卫星所观测的结果以及与采用其他方法得到的结果符合得较好.      

Response of the ionospheric F-region in the Brazilian sector during the super geomagnetic storm in April 2000 observed by GPS

The response of the ionospheric F-region in the equatorial and low latitude regions in the Brazilian sector during the super geomagnetic storm on 06–07 April 2000 has been studied in the present investigation. The geomagnetic storm reached a minimum D_st of −288 nT at 0100 UT on 07 April. In this paper, we present vertical total electron content (VTEC) and phase fluctuations (in TECU/min) from GPS observations obtained at Imperatriz (5.5°S, 47.5°W; IMPZ), Brasília (15.9°S, 47.9°W; BRAZ), Presidente Prudente (22.12°S, 51.4°W; UEPP), and Porto Alegre (30.1°S, 51.1°W; POAL) during the period 05–08 April. Also, several GPS-based TEC maps are presented from the global GPS network, showing widespread and drastic TEC changes during the different phases of the geomagnetic storm. In addition, ion density measurements on-board the satellite Defense Meteorological Satellite Program (DMSP) F15 orbiting at an altitude of 840 km and the first Republic of China satellite (ROCSAT-1) orbiting at an altitude of 600 km are presented. The observations indicate that one of the orbits of the DMSP satellite is fairly close to the 4 GPS stations and both the DMSP F15 ion-density plots and the phase fluctuations from GPS observations show no ionospheric irregularities in the Brazilian sector before 2358 UT on the night of 06–07 April 2000. During the fast decrease of D_st on 06 April, there is a prompt penetration of electric field of magnetospheric origin resulting in decrease of VTEC at IMPZ, an equatorial station and large increase in VTEC at POAL, a low latitude station. This resulted in strong phase fluctuations on the night of 06–07 April, up to POAL. During the daytime on 07 April during the recovery phase, the VTEC observations show positive ionospheric storm at all the GPS stations, from IMPZ to POAL, and the effect increasing from IMPZ to POAL. This is possibly linked to the equatorward directed meridional wind. During the daytime on 08 April (the recovery phase continues), the VTEC observations show very small negative ionospheric storm at IMPZ but the positive ionospheric storm effect is observed from BRAZ to POAL possibly linked to enhancement of the equatorial ionospheric anomaly.     

Effects observed in the ionospheric F-region in the South American sector during the intense geomagnetic storm of 14 December 2006

This investigation presents observations related to the generation of equatorial ionospheric irregularities (also known as equatorial spread F (ESF)) including ionospheric plasma bubbles and dynamic behavior of the ionospheric F-region in the South American sector during an intense geomagnetic storm in December 2006 (a period of low solar activity). In this work, ionospheric sounding observations and GPS data obtained between 13 and 16 December 2006 at several stations in the South American sector are presented. On the geomagnetically disturbed night of 14 and 15 December, ionospheric plasma bubbles were observed after an unusual uplifting of the F-region during pre-reversal enhancement (PRE) period. The unusual uplifting of the F-region during PRE was possibly associated with prompt penetration of electric field of magnetospheric origin. During the geomagnetic disturbance night of 14 and 15 December, strong oscillations due to the propagation of traveling ionospheric disturbances (TIDs) by the Joule heating in the auroral region were observed in the F-region at São José dos Campos (SJC, 23.2°S, 45.9°W; dip latitude 17.6°S), Brazil, and Port Stanley (PST, 51.6°S, 57.9°W; geom. latitude 41.6°S). The VTEC-GPS observations presented on the night of 14 and 15 December 2006 show both positive and negative storm phases in the South American sector, possibly due to changes in the large-scale wind circulation and changes in the O/N₂ ratio in the southern hemisphere, respectively.     

基于二级多点逼近算法的航天器结构优化设计

在某新型卫星结构研制的初样阶段,建立了卫星初始设计的有限元模型.以主承力桁架结构中各梁的截面尺寸为设计变量,考虑整星模态频率和强度约束,建立了以结构重量最轻为目标的优化模型.应用二级多点逼近优化算法进行了结构优化计算,在每一个计算周期中,原结构优化问题先转化为具有较高精度的第1级多点近似问题,该问题则通过可由对偶法快速求解的第2级近似问题逼近.经过初步试算、设计改进和再优化3个阶段,设置并进行了一系列的优化计算,逐步明确了设计的方向和各结构参数的取值范围,得到了合理的可行方案,为该卫星平台结构初样的详细设计提供了参考,同时表明所采用的优化方法适用于工程结构优化问题.      

F-region ionospheric parameters observed in the equatorial and low latitude regions during medium solar activity in the Brazilian sector and comparison with the IRI-2007 model results

The ionospheric sounding observations using the Canadian Advanced Digital Ionosondes (CADIs) operational at Palmas (PAL; 10.2°S, 48.2°W; dip latitude 6.6°S; a near-equatorial station), and São José dos Campos (SJC, 23.2°S, 45.9°W; dip latitude 17.6°S; a low-latitude station located under the southern crest of the equatorial ionospheric anomaly), Brazil, are analyzed during the different seasons viz., winter (June and July 2003), spring (September and October 2003), summer (December 2003 and January 2004), and fall (March and April 2004). The period used has medium solar activity (sunspot number between 77.4 and 39.3). The seasonal mean variations (using only geomagnetically quiet days) of the ionospheric parameters foF2 (critical frequency of the F-region), hpF2 (virtual height at 0.834 foF2; considered to be close to hmF2 (peak height of the F-region)), and h’F (minimum virtual height of the F-region) are calculated and compared between PAL and SJC. The prominent differences between PAL and SJC are as follows: h’F variations show strong post-sunset enhancement at PAL during the seasons of spring, summer, and fall; hpF2 variations show pre-sunrise uplifting of the F-layer at both stations during all the seasons and the hpF2 values during the daytime are lower at SJC compared with PAL during all the seasons; the foF2 variations show mid-day bite-out at PAL during all the seasons and SJC shows strong equatorial ionospheric anomaly during summer and fall seasons. Also, the seasonal variations of the ionospheric parameters foF2 and hpF2 (with ±1 standard deviation) observed at PAL and SJC are compared with the IRI-2007 model results of foF2 and hmF2. In addition, variations of the foF2 and hpF2 observed at SJC are compared with the IRI-2001 model results of foF2 and hmF2. It should be pointed out that the ionospheric parameter hpF2 is much easier to obtain using computer program developed at UNIVAP compared with hmF2 (using POLAN program). During the daytime due to underlying ionization hpF2 estimated is higher (approximately 50 km) than the true peak height hmF2. During the nighttime hpF2 is fairly close to hmF2. The comparison between the foF2 variations observed at PAL and SJC with the IRI-2007 model results shows a fairly good agreement during all the seasons. However, the comparison between the hpF2 variations observed at PAL and SJC with the hmF2 variations with the IRI-2007 model results shows: (1) a fairly good agreement during the nighttime in all the seasons; (2) the model results do not show the pre-sunrise uplifting of the F-layer at PAL and SJC in any season; (3) the model results do not show the post-sunset uplifting of the F-layer at PAL; (4) considering that, in general, hpF2 is higher than hmF2 during the daytime by about 50 km, the model results are in good agreement at PAL and SJC during all the seasons except summer at SJC, when large discrepancies in the observed hpF2 and modeled hmF2 are observed. Also, it has been observed that, in general, hmF2 values for SJC calculated using IRI-2001 are higher than IRI-2007 during the daytime in winter, summer, and fall. However, hmF2 values for SJC calculated using IRI-2001, are lower than IRI-2007 during the nighttime in spring.     

气动磁镜聚变推进器的火星探测任务分析

将气动磁镜聚变概念拓展到空间推进器应用,分析了不同等离子体密度和氢推进剂质量流率下聚变推进器的比冲和推力变化范围,理论计算表明其比冲可达10 000 s以上,推力最高可达几十牛。在此基础上,进一步采用气动磁镜聚变推进器对地火转移任务进行了数值仿真。假设推进器初始质量为100 t,仿真结果表明:当飞行时间在282.42~639.76 d变化时,剩余质量从88.59 t提升至98.24 t。相关分析表明基于气动磁镜的聚变空间推进器通过调节比冲和推力组合方式,可以很好地满足未来火星载人和货运任务对飞行时间和有效载荷份额的不同需求,是未来高性能空间推进器发展的一种候选方案。      

非热压罐预浸料成型技术研究进展

非热压罐成型(out of autoclave process,OoA)技术是实现结构复合材料低成本制造的有效途径,是当前复合材料研究领域的热点之一。本文介绍了OoA成型复合材料国内外的研究前沿以及在航空航天领域的应用现状,从材料体系和成型工艺两大方面总结了OoA成型过程中的缺陷控制方法。在OoA预浸料成型技术中,可通过尽量减少树脂体系中挥发物含量、精细调控树脂体系反应和流变特性、控制预浸料中纤维和树脂的浸润程度、优化成型工艺等手段有效降低复合材料的孔隙率等缺陷。