超声速光学头罩流场的PIV研究

在马赫数Ma-3．8超声速风洞中,采用PIV（Particle Image Velocimetry,粒子图像测速）技术测量了超声速光学头罩流场的速度分布。PIV技术应用于超声速流场时,对系统的硬件配备、示踪粒子的跟随性以及PIV算法的精度有很高的要求。本文PIV系统选用高精度的同步控制器和高能量激光器;以纳米级粒径的粒子作为示踪粒子,通过斜激波响应实验分析了其在超声速流场中的跟随性;并采用多种高精度速度场算法对粒子图像进行处理。实验结果表明,示踪粒子在超声速流场中有很好的跟随性,采用的高精度速度场算法能够很好地反映超声速光学头罩流场的速度分布。     

Old tail lobes effect on the solar-wind – Magnetosphere energy transport for the 27 August 2001 substorm

The magnetic flux of tail lobes Ψ is divided in two parts of comparable values Ψ₁ and Ψ₀₂, with the first that appears during substorm and the second, observed before substorm start. The first was named “new magnetic flux”, the second – “old magnetic flux”. The first, Ψ₁, is known to play a definitive role in the energy transport from the solar wind into the magnetosphere-ionosphere-atmosphere system, but the role of Ψ₀₂ in this transport is not well known. From the 27 August 2001 substorm data we study the involvement in the above transport process of the old flux Ψ₀₂. This involvement is observed in the polar cap (PC) area, which existed prior to the substorm and is called respectively “the old PC”. In this study, as distinct from earlier works, we use the balance equation of the energy stored in magnetosphere and energy consumed. Activation of the old PC magnetic flux Ψ₀₂ was found to increase the energy input by ∼85% in the event under consideration.     

Mechanical properties of ANTRIX balloon film and fabrication of single cap large volume balloons

The zero pressure plastic balloons used for high altitude studies are generally made from polyethylene material. Tensile properties of the thin film polymer are the key parameters for material selection due to extremely low temperature of −90 °C encountered by the balloons in the tropopause region during the ascent at equatorial latitudes. The physical and structural properties of the material determine the uniformity of the stress distribution over the entire shell. Load stresses from the suspended load propagate via load tapes heat sealed along with the gore seals as per the balloon design. A balance between this heat seal strength and the film strength is a desirable property of the basic resin in terms of the bubble strength, gauge uniformity, and long-term storage properties. In addition, the design of the top shell of the balloon and its stress distribution play an important role since only a fraction of the balloon is deployed during the filling operation and the ascent. In this paper we describe the mechanical properties of the ‘ANTRIX’ film developed by us and the optimized design of single cap balloons, which have been successfully used in our experiments over the past 5 years.     

Winter cross polar cap current estimation

Digital ionosonde and magnetometer observations from a polar cap station are used to estimate the fraction of Region 1 current that flows across the polar cap. For a winter case study using data for 2001 Feb 18 the cross-cap current was 3.9 × 10⁴ A Pedersen current and 6 × 10⁴ A Hall current. This total current is only a small percentage, ∼5%, of the Region 1 current.     

某型雷达高压帽模压硫化成型法制作探讨

制作某型雷达高压帽时,针对试制品出现分型面不同程度的撕裂情况,经请教相关专家和综合分析,得出该橡胶制品出现撕裂与模具结构以及硫化制作工艺有关.在对模具结构和硫化工艺进行分析改进后制出合格产品,经国家橡胶密封制品质量监督检验中心性能检验,性能均达到技术指标要求,装备使用两年来安全可靠.此次制作成功为今后更好地开展橡胶件制...     

某型飞机端盖的失效分析

采用扫描电子显微镜(SEM)、能谱分析(EDS)和显微硬度(MHV)测试等手段对某型飞机的Al-Si-Cu铸造合金端盖进行了失效分析.结果表明:在交变载荷的长期作用下,端盖凸缘处材料出现了裂纹.裂纹的存在引起了应力集中,最终导致了零件的疲劳断裂.     

月球车刚性车轮与模拟月壤相互作用有限元仿真和试验验证

根据三轴试验结果获得了模拟月壤的模型参数,在ABAQUS中基于修正的Drucker Prager Cap弹塑性模型建立了模拟月壤的仿真模型,并通过仿真的压板沉陷试验对试验测到的模型参数进行校正,然后基于该模型对月球车刚性车轮和模拟月壤的相互作用进行了仿真分析和试验验证,结果发现牵引力的计算结果在低滑转率下和试验结果复合较好,而在高滑转率下,计算结果偏大。最后对不同土壤自重下单个月球车车轮的牵引性能变化进行了仿真分析,发现单是土壤自重的变化对车轮牵引性能影响不明显。     

不同几何结构对燃油喷嘴热防护特性的影响

试验研究了不同管路结构对燃油结焦性能的影响,结果表明,在1 000 K、150 m/s来流条件和400 K、05 m/s燃油条件下,减小弯管角度和突扩管路的突扩尺寸可以降低结焦附着,且在对管路加热的初始阶段中,结焦量随时间增加会出现波动,在加热15 min时管壁结焦量达到最大,壁面上部分结焦的脱落使结焦量降低。随后,采用试验与数值模拟相结合的方法研究了喷嘴和喷嘴帽罩结构对热防护特性的影响。结果表明,主、副油路同心布置的喷嘴具有最好的热防护效果,在所试验工况下最高可降低湿壁温度近50%,甚至优于带空气隔热层的模型。而喷嘴帽罩对喷嘴出口油温的降低有限,但减小帽罩与喷嘴体的接触或在接触面处填充低热导率的材料仍是有效的改进措施,可降低出口油温约5 K。研究结果对喷嘴的热防护设计具有指导作用。     

Azimuthal propagation of Pc5 geomagnetic field pulsations in the southern polar cap

A statistical analysis of low frequency geomagnetic fluctuations at the two Antarctic stations Mario Zucchelli Station (geographic coordinates: 74.7°S, 164.1°E; corrected geomagnetic coordinates: 80.0°S, 306.8°E) and Dumont D’Urville (geographic coordinates: 66.7°S, 140.0°E; corrected geomagnetic coordinates: 80.4°S, 236.0°E) is shown. The analysis focuses on power spectra, coherence and phase difference between the stations, which are both located in the polar cap, with a 5-h magnetic local time displacement along a geomagnetic parallel; in this situation, the phase difference between geomagnetic fluctuations indicates the direction of their azimuthal propagation. Coherent fluctuations have been found to occur preferably when both stations are on the same side (dawnward or duskward) with respect to the polar cusp; moreover, around local magnetic midnight, they occur essentially during open magnetospheric conditions. The phase difference for coherent fluctuations indicates a propagation direction away from local geomagnetic noon and midnight. Also the analysis of three individual pulsation events, occurring at different times during the day, is shown; they are characterized at the two stations by simultaneous, coherent fluctuations, whose phase difference finds correspondence with the statistical behaviour.     

Variations in polar rain flux according to IMF geometries observed by STSAT-1

We examined polar rain flux observed by STSAT-1 in the northern polar cap and compared it with solar wind parameters. We found that the differential energy spectrum of polar rain was similar to that of the solar wind for the energy range 100 eV – 1 keV, although we cannot rule out the possibility of a small amount of acceleration. On the other hand, the low-energy component of the solar wind showed no correlation and, naturally, the solar wind density had only a weak correlation with the polar rain flux. Polar rain flux in the northern hemisphere is most significant for the condition of the interplanetary magnetic field components Bz < 0, Bx < 0, and By > 0, and in this case it correlated well with the magnitude of By and Bz. For other interplanetary magnetic field conditions, the correlation was insignificant. The results are consistent with those reported previously.