组分变化对甲烷氧化特性影响

在射流搅拌反应器实验平台上针对温度范围850~1 300 K、常压条件下的甲烷氧化反应过程进行了实验研究,采用气相色谱仪测量了变组分条件下(当量比范围02~2、氧气体积分数2%~8%、二氧化碳体积分数0~20%、水蒸气体积分数0~20%)主要反应物(CH4、O2)、主要中间组分(C2H6、C2H4、C2H2、H2)和主要污染物(CO、CO2)的摩尔分数,并分析了主要反应物、中间组分以及污染物生成的影响因素和影响规律。研究表明,随着当量比和含氧量的增加,主要中间组分的摩尔分数升高;二氧化碳体积分数的增加对中间产物的生成有微弱的抑制作用,却使得污染物浓度大大增加;水蒸气体积分数的增加导致氢气生成量显著增加,同时促进一氧化碳的生成,而对二氧化碳的生成影响很小。      

并联混合动力齿轮传动涡扇发动机建模与性能分析

为对比探究未来大推力航空混合动力系统与传统航空发动机的优劣,本文依托某概念型齿轮传动涡扇(Geared turbofan,GTF)发动机,设计了一个并联航空油-电混合动力系统(hybrid GTF,hGTF),在Matlab /Simulink数字仿真软件中建立相匹配的电动力模型以及氮氧化物NOx排放和噪声预测等性能参数计算模型,并在稳态和飞行任务剖面下初步分析了电动力系统的引入对原基线GTF发动机的性能改变状况。稳态仿真结果表明,大推力等级的并联油-电混合动力系统中,至少需要兆瓦级的电动力系统进行匹配;当电动力系统处于电动模式时,可能会带来低压压气机喘振的隐患;当电动力系统处于再生模式时,电能源相当于经过了电能到机械能再到电能的二次效率损失,不建议采用。飞行任务剖面动态仿真结果表明,相比于传统GTF发动机,hGTF推进系统的燃油消耗率最高下降15%,总燃油消耗节省8.3%, NOx总排放量减少18.8%,各部件起飞噪声总声压级减少1.5~3.3dB。分析结果表明采用并联混合动力系统具有显著提升省油、减排效果的能力,同时也具有一定的降噪潜力。     

刚性太阳电池阵基板的研究

文章简要地叙述碳纤维复合材料刚性太阳电池阵基板的结构设计,理论分析,模态试验和振动试验。理论分析和试验结果比较一致。通过试验还解决了基板各种复合材料的力学性能测试问题,取得了必要的数据。     

捕获加速新生离子对Alfvén波的激发

根据准线性方程,求出了在离子持续产生并被太阳风捕获加速的情况下离子的渐近态分布函数.采用此分布函数分析了斜向传播的Alfven波的稳定性.     

卫星地面接收站电磁环境的测试和分析

对卫星地面站电磁环境的测试进行介绍和分析,着重论述了测试系统、测试技术、测试中的经验及所遇到的问题。     

空间站大面积太阳翼热分析

本文在一定的假设条件下，对空间站大面积太阳翼进行了系统的热流和温度场计算。在计算中利用矢量分析和坐标变换的方法求解出了太阳直接辐射1地球红外辐射和地球反照的辐射角系数，再根据传热学理论建立了瞬态热平衡方程，应用有限单元法对热平衡方程进行了求解。本文通过计算给出了各项热流的大小及在总热流中所占的比例和太阳民办的瞬态温度场分布，对空间站大面积太阳翼设计及热控制具有一定的参考价值。     

模型燃烧室中两相化学反应流动的大涡模拟

对带V型火焰稳定器的模型燃烧室中气液两相化学反应流动进行大涡模拟(LES),研究中采用了欧拉一拉格朗日方法。利用大涡模拟来研究气相流场,k方程亚网格尺度模型来模拟亚网格涡粘性。化学反应速率由亚网格EBU燃烧模型来确定,两步亚网格紊流燃烧模型被用来确定CO浓度,NO亚网格污染物生成模型被用来评估NO生成速率,辐射热量传递采用了热通量辐射模型。并在交错网格体系下气相采用SIMPLE算法和混合差分格式求解,液相在拉格朗日坐标系下采用PSIC算法对其进行求解。通过大涡模拟,能得到气相和液相之间的质量、动量和能量交换。通过计算值和实验值的比较可知,出口温度和污染物成分浓度实验结果与计算结果吻合较好。因此采用大涡模拟方法来模拟两相化学反应流动和污染物生成过程是可行的。     

广州地磁Z分量日变幅的谱特征

利用1972—1993年广州地磁资料，分析了Z分量日变幅的年平均、年变化和半年变化等低频成分的逐年变化，以及小于60天的短周期变化特征．同时对1972—1993年的F10.7日均值进行了谱分析．结果指出，广州地磁Z分量日变幅的年平均与太阳活动指数F10．7的年平均存在良好的线性相关；具有幅度大约5nT夏季极大的年变化，与太阳活动没有明显相关，是一种季节效应；存在春秋分极大的半年变化，幅度与太阳活动有关，高年的幅度明显大于低年；具有明显的与太阳自转相关的27天左右的变化和明显的与行星波有关的接近16日、10日、5日、2日等短周期变化．广州地磁Z分量日变幅的这些谱特征，有助于更深入地了解中低层大气对电离层影响的物理机制．     

Interplanetary shocks and sudden impulses during solar maximum (2000) and solar minimum (1995–1996)

In this work a study is performed on the correlation between fast forward interplanetary shock parameters at 1 Astronomical Unit and sudden impulse (SI) amplitudes in the H-component of the geomagnetic field, for periods of solar activity maximum (year 2000) and minimum (year 1995–1996). Solar wind temperature, density and speed, and total magnetic field, were taken to calculate the static pressures (thermal and magnetic) both in the upstream and downstream sides of the shocks. The variations of the solar wind parameters and pressures were then correlated with SI amplitudes. The solar wind speed variations presented good correlations with sudden impulses, with correlation coefficients larger than 0.70 both in solar maximum and solar minimum, whereas the solar wind density presented very low correlation. The parameter better correlated with SI was the square root dynamic pressure variation, showing a larger correlation during solar maximum (r = 0.82) than during solar minimum (r = 0.77). The correlations of SI with square root thermal and magnetic pressure were smaller than with the dynamic pressure, but they also present a good correlation, with r > 0.70 during both solar maximum and minimum. Multiple linear correlation analysis of SI in terms of the three pressure terms have shown that 78% and 85% of the variance in SI during solar maximum and minimum, respectively, are explained by the three pressure variations. Average sudden impulse amplitude was 25 nT during solar maximum and 21 nT during solar minimum, while average square root dynamic pressure variation is 1.20 and 0.86 nPa^1/2 during solar maximum and minimum, respectively. Thus on average, fast forward interplanetary shocks are 33% stronger during solar maximum than during solar minimum, and the magnetospheric SI response has amplitude 20% higher during solar maximum than during solar minimum. A comparison with theoretical predictions (Tsyganenko’s model corrected by Earth’s induced currents) of the coefficient of sudden impulse change with solar wind dynamic pressure variation showed excellent agreement, with values around 17 nT/nPa^1/2.     

Research on a complex CME event including Hα, LASCO, radio and MDI observations

We present our research on a fast and decelerating partial halo coronal mass ejection (CME) event detected in multi-wavelengths in the chromosphere and the corona on 14 October, 1999. The event involved a whole complex active area which spanned more than 40° of heliolongitude. It included a strong solar flare (XI/1N) and a complex eruptive filament within an active region of the entire complex. Especially, several radio sources were detected in the decimetric range prior to the CME by the Nançay Radioheliograph (NRH). A linear force-free field extrapolation of the Michelson Doppler Imager (MDI) magnetogram was performed to calculate the magnetic topology of the complex prior to the triggering of the event. The presence of a coronal null point combined with the occurrence of two distant and nearly simultaneous radio sources put strong arguments in favor of the generalized breakout model for the triggering of the eruption. The analysis of the subsequent development of the event suggests that large interconnecting loops were ejected together with the CME.