太阳10.7cm射电流量中期预报模型研究(Ⅰ)

采用时间序列模型中的自回归方法开展了F_(10.7)中期预报研究.预报试验和误差分析结果表明,在太阳活动水平较低、F_(10.7)的27天周期性明显时自回归预报方法的预报精度高,具有较为理想的预报效果,但在日面有大活动区产生和消亡时预报效果不理想.这说明时间序列模型中的自回归方法能够较好地反映太阳F_(10.7)的27天周期性特征,对F_(10.7)中期预报模型的建立有一定适用性.通过对2005年9月21日至2007年6月7日期间预报结果的比较可以看出,自回归分析方法预报的精度与美国空军预报的相当。     

弯曲/倾斜叶片对大展弦比涡轮气动性能影响

为了获得弯曲/倾斜导叶对大展弦比低压涡轮气动性能的影响,通过求解基于耦合转捩SST湍流模型的雷诺平均N-S方程组,对GE-E3低压涡轮叶栅的进行了全三维粘性定常与非定常数值模拟。研究了弯曲/倾斜导叶对涡轮级效率的影响,分析了对导叶叶栅气动性能、导叶扩散因子与边界层发展的作用,以及对下游动叶气动性能和动叶吸力面流动特性的影响。结果表明,正弯导叶减小了二次流损失却带了更大的叶型损失,降低了涡轮级效率,而正倾斜改变了上下端壁的二次流损失分配,对总的叶型损失影响较小,在一定角度下能够改善大展弦比涡轮叶栅的气动性能。     

改进升力线理论和风洞试验结合的气动弹性修正方法

本文介绍了一种基于亚音速稳态定常流改进升力线理论与风洞试验相结合的大展弦比亚音速飞机的弹性翼面气动力分布载荷修正方法,设计目的是为了考虑具有大展弦比、弹性翼面结构的飞机翼面结构弹性变形对气动载荷分布的影响。     

宽高比及表面粗糙度对矩形微尺度通道流动特性的影响

实验研究了不同宽高比矩形金属微尺度通道的流动特性,并与硅通道对比来探究表面粗糙度的影响。金属微尺度通道宽为0.4mm,通道宽高比分别为0.50、0.67、和1.00,相对表面粗糙度范围为0.1609%~0.2145%。硅通道宽度及高度都为0.4mm,相对表面粗糙度为0.00325%。实验工质为空气,实验的雷诺数范围是250~3000。实验结果表明:在粗糙微尺度通道会发生转捩提前,并且转捩雷诺数随着宽高比增大而减小。在层流区,微尺度矩形通道摩擦因数随着雷诺数增大而减小,在转捩区出现明显增大后再减小。表面粗糙度很小时,未发现转捩提前现象。      

考虑气动力非线性的柔性飞机阵风响应分析

针对大展弦比柔性飞机阵风响应问题,考虑在大攻角(AOA)情况下气动力非线性的影响,通过将修正的Theodorsen方法与片条理论相结合,得到非线性的时域非定常气动力;在此基础上,建立阵风干扰下的大展弦比柔性飞机非线性气动弹性模型,完整地发展了一种新颖的可考虑气动力非线性的大展弦比柔性飞机阵风响应分析方法.结合算例模型开展方法验证和数值仿真,对比翼尖和质心(CG)处阵风附加过载在线性和非线性情况下的变化.算例结果表明,考虑大攻角情况下的气动力非线性后,大展弦比飞机的阵风响应较线性情况有明显变化,翼尖处的阵风附加过载最多可减少41.7%,气动力非线性的影响不可忽视.      

改进 K-均值算法在雷达辐射源信号预分选中的应用

雷达辐射源信号分选是电子对抗领域一个关键技术,随着电子技术的发展,电磁环境日趋复杂,信号分选的难度越来越大,在这样的条件下,我们应该寻求新的解决问题的方法.本文首先概述了雷达辐射源信号分选意义、系统组成和分选流程,然后介绍了改进 K-均值算法.为了有效实现信号分选,提出了基于改进K-均值算法的信号分选方法,该方法可对到达角、载频和脉宽参数进行分选.最后进行了仿真实验,结果表明该方法实现简单,分选效果较好     

An alternative Shell inversion technique - Analysis and validation based on COSMIC and ionosonde data

Multi-channel Global Positioning System (GPS) carrier phase signals, received by the six low Earth orbiting (LEO) satellites from the Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) program, were used to undertake active limb sounding of the Earth’s atmosphere and ionosphere via radio occultation. In the ionospheric radio occultation (IRO) data processing, the standard Shell inversion technique (SIT), transformed from the traditional Abel inversion technique (AIT), is widely used, and can retrieve good electron density profiles. In this paper, an alternative SIT method is proposed. The comparison between different inversion techniques will be discussed, taking advantage of the availability of COSMIC datasets. Moreover, the occultation results obtained from the SIT and alternative SIT at 500 km and 800 km, are compared with ionosonde measurements. The electron densities from the alternative SIT show excellent consistency to those from the SIT, with strong correlations over 0.996 and 0.999 at altitudes of 500 km and 800 km, respectively, and the peak electron densities (N_mF₂) from the alternative SIT are equivalent to the SIT, with 0.839 vs. 0.844, and 0.907 vs. 0.909 correlation coefficients when comparing to those by the ionosondes. These results show that: (1) the N_mF₂ and h_mF₂ retrieved from the SIT and alternative SIT are highly consistent, and in a good agreement with those measured by ionosondes, (2) no matter which inversion technique is used, the occultation results at the higher orbits (∼800 km) are better than those at the lower orbits (∼500 km).     

一种航天器单脉冲差模角跟踪系统的标定及测试方法

介绍了航天器单脉冲差模角跟踪系统的组成和基本原理;针对捕获跟踪系统性能与射频通道相位特性的相关性,提出了在无线状态下通过用户目标在一定范围内按一定轨迹运动进行射频通道相位标定及跟踪性能测试的方法;在此基础上进一步提出了利用信号源模拟用户目标在角跟踪系统天线坐标系下不同位置时天线输出的射频信号,进行有线状态下射频通道性能的测试方法。标定及测试方法通过地面试验验证了可行性和有效性,可用于航天器单脉冲差模角跟踪系统在地面的通道相位标定、跟踪性能测试和射频通道性能测试,以实现角跟踪系统对用户目标高精度、稳定的跟踪。     

Low-latitude ionospheric scintillations and total electron content obtained with the CITRIS instrument on STPSat1 using radio transmissions from DORIS ground beacons

The primary objective of the Scintillation and Tomography Receiver in Space (CITRIS) is to detect ionospheric irregularities from space at low latitude. For this purpose, the satellite receiver uses the UHF and S-Band transmissions of the ground network of Doppler Orbitography and Radiopositioning Integrated by Satellite (DORIS) beacons. CITRIS, developed at the Naval Research Laboratory, differs from the normal DORIS receiver by being able to capture and store the complex amplitude of the 401.25 and 2036.25 MHz transmissions at 200 Hz sample rate. Ground processing of the CITRIS data yields total electron content (TEC) and both phase and amplitude scintillations. With CITRIS flying on the US Space Test Program (STP) satellite STPSat1, 2 years of data were collected and processed to determine the fluctuations in ionospheric TEC and radio scintillations associated with equatorial irregularities. CITRIS flights over DORIS transmitters yield direct measurements of the horizontal plasma density fluctuations associated with equatorial plasma bubbles. Future flights of CITRIS can provide valuable complements to other satellite instruments such as GPS occultation receivers used to estimate vertical electron density profiles in the ionosphere.     

Height of shock formation in the solar corona inferred from observations of type II radio bursts and coronal mass ejections

Employing coronagraphic and EUV observations close to the solar surface made by the Solar Terrestrial Relations Observatory (STEREO) mission, we determined the heliocentric distance of coronal mass ejections (CMEs) at the starting time of associated metric type II bursts. We used the wave diameter and leading edge methods and measured the CME heights for a set of 32 metric type II bursts from solar cycle 24. We minimized the projection effects by making the measurements from a view that is roughly orthogonal to the direction of the ejection. We also chose image frames close to the onset times of the type II bursts, so no extrapolation was necessary. We found that the CMEs were located in the heliocentric distance range from 1.20 to 1.93 solar radii (Rs), with mean and median values of 1.43 and 1.38 Rs, respectively. We conclusively find that the shock formation can occur at heights substantially below 1.5 Rs. In a few cases, the CME height at type II onset was close to 2 Rs. In these cases, the starting frequency of the type II bursts was very low, in the range 25–40 MHz, which confirms that the shock can also form at larger heights. The starting frequencies of metric type II bursts have a weak correlation with the measured CME/shock heights and are consistent with the rapid decline of density with height in the inner corona.