微藻反应器用于水气净化与产氧的功能验证

将微藻和电去离子技术引入密闭生态系统,设计单元反应器旨在验证其在空气再生、水净化和潜在食物的生产。在反应器中对尿液进行消解和NH4＋硝化转化得到超过90%NH4＋-N硝化为NO-3-N-的培养液适宜于螺旋藻养殖并获得高质量的微藻生物量;此时,CO2的平均吸收速率VCO2=458.6 mL/m3·min、O2产生速率VO2=616.5 mL/m3·min,即螺旋藻的同化系数VCO2/VO2≈0.74,接近人的呼吸系数VCO2/VO2=0.86;EDI法水净化率97%可直接回用。结果表明：该体系能实现CO2吸收、O2释放和螺旋藻生物量的生产,同时将水净化。     

装备激励约束定价模式机理对比分析与设计

激励约束定价模式能够极大调动承包商积极性，是控制装备成本的一种重要方法。通过深入分析美军激励约束定价模式和我军激励约束定价模式的设计机理，提出了承包商的期望利润和军方期望价格的计算方法，并通过对比不同定价模式的特点，在借鉴2种激励约束定价模式优点基础上，设计了一种新的激励约束定价策略，提出了指导装备激励约束定价模式改革的对策建议。最后，通过算例对本文方法进行了解释，同时验证了本文方法的有效性。     

机载综合无线电平台的中频数据传输总线优选分析

在综合无线电平台中，根据硬件平台通用化要求，需要选择一种总线同时满足CNI 不同波形的中频 数据传输对延时、带宽和误码率的要求。本文针对不加协议的GTX 和加上高速串行通信协议的Aurora、SRIO 进行测试，得到这三种高速串行总线在延时、带宽和误码率的对比分析，从而选择一种总线作为多波形综合的 中频数据传输总线。     

基于多尺度 3D-2D卷积神经网络的高光谱图像分类

设计提出了 1种针对高光谱图像分类任务的 3D-MSCNN模型。在 PCA降维的基础上,利用 3D空谱特征提 取网络和 2D多尺度特征提取网络实现高光谱图像特征提取,充分发挥高光谱图像空谱信息价值,增强对不同尺度 地表覆盖的表达能力。最后,利用 Softmax分类损失函数实现高光谱图像分类任务。实验结果表明,本文算法在 In. dian Pines和 Pavia University数据集上都取得了较好的分类效果。与 CD-CNN、3D-CNN、SS-Net和 HybirdSN等方法相 比,本文算法能够有效提升总体精度、平均精度和 Kappa系数等客观评价指标。     

以可用度为目标的民用飞机不完全预防性维修间隔优化

民用飞机制造商推荐的初始预防性维修间隔通常不考虑运营环境和维修能力的差异,在满足飞机安全性要求的同时,难以达到可用性的最优状态。基于不完全维修理论,采用役龄回退因子修正部件的可靠性模型,以反映维修工作对于部件性能的影响;结合航空公司运行实际情况,以部件可用度为目标函数,可靠度阈值为约束条件,提出不完全维修策略下的预防性维修间隔优化模型,并以某型飞机的空气起动机航线故障数据进行实例验证。结果表明：在满足可靠度阈值的约束条件下,所建立的维修间隔优化模型得出的最优维修间隔与实际相符,该模型合理可行。     

驻涡燃烧室前钝体燃料喷射性能数值分析

为研究驻涡燃烧室在前钝体燃料喷射状况下的燃烧性能,采用3维数值仿真模拟方法,对驻涡燃烧室前钝体燃料喷射 状况下的燃烧效率及燃烧室性能与无前钝体燃料喷射状况下的燃烧性能进行了对比分析,并对驻涡燃烧室的冷流以及燃烧状态 下的燃烧室性能进行了系统研究。燃烧室温度分布表明：前钝体顶部燃料喷射在0.2~0.7的喷射系数范围内,缩短了燃烧室火焰 长度,提高了燃烧室在相同轴向长度下的燃烧效率,使燃烧室更加紧凑;驻涡燃烧室前钝体顶部燃料喷射孔的孔径在一定范围内 的变化对燃烧室的燃烧效率、出口温度分布系数以及总压损失影响较小。     

超临界碳氢燃料蒸汽重整一维模型研究

为了获得关键参数对超临界碳氢燃料蒸汽重整化学热沉分布特性的影响,建立了超临界碳氢燃料蒸汽重整非稳态一维计算模型,通过与实验数据的对比验证了模型的准确性,并基于该模型采用RP-3的四组分替代模型对RP-3蒸汽重整过程中入口流速、压力和含水量等关键参数对热沉沿流向分布特性的影响进行了研究。结果表明：随着入口流速的增加,蒸汽重整反应化学热沉的峰值减小,且出现峰值的位置逐渐向出口移动。随着压力的升高,相同位置处的化学热沉都减少,但是出现峰值的位置不变。在入口含水量由5%增大到12%的过程中,微通道同一位置处的化学热沉增大,且化学热沉的最大值也是增大的,峰值出现的位置向微通道出口移动。     

延伸冲击孔冲击冷却流动与换热特性的数值研究

采用数值模拟方法研究了延伸冲击孔冲击冷却系统的冷却特性,分析了3个冲击雷诺数和5个冲击孔延伸长度对冲击腔内流动与换热特性的影响,给出了靶面努塞尔数分布、靶面压力分布、中心截面流速与综合换热性能的变化。结果表明：延伸冲击孔可以有效地防止横流对冲击射流的偏转作用,同时使射流出口更加贴近冲击靶面壁面,冲击速度更高,可以明显提高靶面的换热系数,并使整个靶面上的换热系数分布也更加均匀。冲击冷却的冷却性能随着冲击孔延伸长度的增加而增加,相较于传统冲击冷却（baseline）,在L/d=2.5时靶面平均努塞尔数提升达15%以上,但压力损失也相对较高;对比不同延伸长度冲击孔的综合换热性能,发现存在最佳的L/d取值范围使冲击冷却系统获得最佳的综合冷却性能。在本研究范围内,最佳的L/d= 2.5。     

Interplanetary origin of geomagnetic storms

Around solar maximum, the dominant interplanetary phenomena causing intense magnetic storms (Dst<−100 nT) are the interplanetary manifestations of fast coronal mass ejections (CMEs). Two interplanetary structures are important for the development of storms, involving intense southward IMFs: the sheath region just behind the forward shock, and the CME ejecta itself. Whereas the initial phase of a storm is caused by the increase in plasma ram pressure associated with the increase in density and speed at and behind the shock (accompanied by a sudden impulse [SI] at Earth), the storm main phase is due to southward IMFs. If the fields are southward in both of the sheath and solar ejecta, two-step main phase storms can result and the storm intensity can be higher. The storm recovery phase begins when the IMF turns less southward, with delays of ≈1–2 hours, and has typically a decay time of 10 hours. For CMEs involving clouds the intensity of the core magnetic field and the amplitude of the speed of the cloud seems to be related, with a tendency that clouds which move at higher speeds also posses higher core magnetic field strengths, thus both contributing to the development of intense storms since those two parameters are important factors in genering the solar wind-magnetosphere coupling via the reconnection process. During solar minimum, high speed streams from coronal holes dominate the interplanetary medium activity. The high-density, low-speed streams associated with the heliospheric current sheet (HCS) plasma impinging upon the Earth's magnetosphere cause positive Dst values (storm initial phases if followed by main phases). In the absence of shocks, SIs are infrequent during this phase of the solar cycle. High-field regions called Corotating Interaction Regions (CIRs) are mainly created by the fast stream (emanating from a coronal hole) interaction with the HCS plasma sheet. However, because the B_z component is typically highly fluctuating within the CIRs, the main phases of the resultant magnetic storms typically have highly irregular profiles and are weaker. Storm recovery phases during this phase of the solar cycle are also quite different in that they can last from many days to weeks. The southward magnetic field (B_s) component of Alfvén waves in the high speed stream proper cause intermittent reconnection, intermittent substorm activity, and sporadic injections of plasma sheet energy into the outer portion of the ring current, prolonging its final decay to quiet day values. This continuous auroral activity is called High Intensity Long Duration Continuous AE Activity (HILDCAAs). Possible interplanetary mechanisms for the creation of very intense magnetic storms are discussed. We examine the effects of a combination of a long-duration southward sheath magnetic field, followed by a magnetic cloud B_s event. We also consider the effects of interplanetary shock events on the sheath plasma. Examination of profiles of very intense storms from 1957 to the present indicate that double, and sometimes triple, IMF B_s events are important causes of such events. We also discuss evidence that magnetic clouds with very intense core magnetic fields tend to have large velocities, thus implying large amplitude interplanetary electric fields that can drive very intense storms. Finally, we argue that a combination of complex interplanetary structures, involving in rare occasions the interplanetary manifestations of subsequent CMEs, can lead to extremely intense storms. This revised version was published online in June 2006 with corrections to the Cover Date.     

三角翼俯仰滚转耦合运动气动特性研究

介绍一套用于３ｍ 低速风洞的俯仰滚转两自由度大振幅非定常实验系统,并利用该系统对—三角翼单独俯仰和滚转及俯仰滚转耦合运动时的非定常气动特性进行了研究。结果表明,飞行器俯仰滚转耦合运动时的气动特性比单独俯仰和滚转时的气动特性复杂得多。