槽道湍流的法向与展向电磁力壁面减阻

法向与展向电磁力可以有效调制湍流近壁流动及减少壁面摩擦阻力.为进一步揭示该方法的减阻机理,利用Fourier-Chebyshev谱方法,通过直接数值模拟(DNS),对槽道湍流的法向与展向电磁力控制和减阻问题进行了研究.结果表明,对于确定的流向波长λx+,存在最佳的电磁力强度St,使阻力降最大,最佳St与λx+成反比.法向与展向电磁力对湍流的控制过程实质上是一种由电磁力诱导的调制波对壁湍流的调制过程.在优化参数控制下,当法向与展向电磁力诱导的流场被用来调制固有的近壁湍流流场时,固有流场和诱导流场同时受到调制.在这种调制波作用下,调制流场逐渐主宰壁面边界层,这导致了壁面阻力的下降,平均减阻率最高可达8％.     

发射脉冲载波泄漏抑制研究与实现

对发射端采用双平衡正交调制器产生线性调频造成载波泄漏的原因进行了详细分析,提出了采用直接数字合成(DDS)技术产生发射端线性调频信号的实现方法,从而很好地解决了载波泄漏的问题,并给出了试验结果。     

HP8902A自动检定系统的研制

介绍了以HP8902A测量接收机为主构成信号源、调制测量仪等仪器的自动检定系统,详细讲述了该系统的构成和软件的实现。     

基于维特比算法的GMSK信号非相干解调技术研究

GMSK体制是深空通信中的新型体制,它具有恒定的包络、优秀的频谱利用率和功率利用率。研究基于维特比算法的GMSK信号非相干解调技术,并在高斯白噪声信道下进行性能仿真。仿真结果表明,该解调算法性能优越,在信噪比Eb/N0=9dB时,GMSK(BT=0.5)信号的误码率性能可达10-4量级,优于传统调频方式约2.4dB。该解调算法已经在某深空测控演示系统中得到了试验验证,性能良好。     

细节信息容量与MTF相关分析

文章从信息容量的角度出发,对图像宏观质量做出评价,再通过研究图像的细节信息容量参数,对在宏观上质量相当的图像做出更进一步的评价,挑选出边缘清晰、纹理等细节信息丰富的图像。然后将该评价参数与Ealing仪测得的调制传递函数(MTF)值的变化趋势作曲线回归分析,实验结果表明,细节信息容量与数字成像系统的MTF值的变化有着很好的正相关关系,这对评价数字成像系统MTF变化情况具有较好的实际应用价值。     

螺旋桨目标的雷达回波信号相位解缠技术

建立了螺旋桨的雷达回波信号模型。对模型回波信号的相位混叠效应进行了理论分析,讨论了回波相位混叠效应出现的原因,通过模型改进获得了螺旋桨的雷达回波相位的理论表达式。提出插值与可调门限相结合的算法和自适应数值积分算法两种相位解缠方法,分别用于桨叶数为偶数和奇数时的相位解缠。仿真结果表明:两种算法有较高的精度。     

Modelling of galactic Carbon in an asymmetrical heliosphere: Effects of asymmetrical modulation conditions

Observations of galactic cosmic rays (GCRs) from the two Voyager spacecraft inside the heliosheath indicate significant differences between them, suggesting that in addition to a possible global asymmetry in the north–south dimensions (meridional plane) of the heliosphere, it is also possible that different modulation (turbulence) conditions could exist between the two hemispheres of the heliosphere. We focus on illustrating the effects on GCR Carbon of asymmetrical modulation conditions combined with a heliosheath thickness that has a significant dependence on heliolatitude. To reflect different modulation conditions between the two heliospheric hemispheres in our numerical model, the enhancement of both polar and radial perpendicular diffusion off the ecliptic plane is assumed to differ from heliographic pole to pole. The computed radial GCR intensities at polar angles of 55° (approximating the Voyager 1 direction) and 125° (approximating the Voyager 2 direction) are compared at different energies and for both particle drift cycles. This is done in the context of illustrating how different values of the enhancement of both polar and radial perpendicular diffusion between the two hemispheres contribute to causing differences in radial intensities during solar minimum and moderate maximum conditions. We find that in the A > 0 cycle these differences between 55° and 125° change both quantitatively and qualitatively for the assumed asymmetrical modulation condition as reflected by polar diffusion, while in the A < 0 cycle, minute quantitative differences are obtained. However, when both polar and radial perpendicular diffusion have significant latitude dependences, major differences in radial intensities between the two polar angles are obtained in both polarity cycles. Furthermore, significant differences in radial intensity gradients obtained in the heliosheath at lower energies may suggest that the solar wind turbulence at and beyond the solar wind termination shock must have a larger latitudinal dependence.     

低频靶标法测量CCD相机调制传递函数的仿真

基于用高频靶标法测试调制传递函数(MTF)时不能准确地体现出CCD器件的平均采样的情况。该文探讨用低频靶标法测试MTF,介绍它的原理;通过数字仿真CCD的光学镜头的模糊和采样平均过程,分析不同频率靶标的MTF测试结果,并分析相位造成的影响。     

Three-dimensional cosmic-ray simulations: Heliographic latitude and current-sheet tilt

We present the results from a study of the variations of the cosmic-ray intensity with time, heliographic latitude, and longitude, and for varying interplanetary conditions, using our three-dimensional, time-dependent computer code for cosmic-ray transport in the heliosphere. Our code also produces a solar-wind and interplanetary magnetic field (IMF) configuration which is compared with observations. Because of the fully threedimensional nature of the model calculations, we are able to model time variations which would be expected to be observed along Ulysses's trajectory as it moves to high latitudes. In particular we can model the approximately 13-and 26-day solar-rotation induced variations in cosmic rays, solar wind and IMF, as a function of increasing heliographic latitude, as one moves poleward of the interplanetary current sheet. Our preliminary model results seem to be in general form quite similar to published data, but depend on the physical parameters used such as cosmic-ray diffusion coefficients, boundary conditions, and the nature of the solar wind and IMF and current sheet.