基于经验模型的对转风扇噪声预测分析

以CF6-80C2发动机风扇和自行设计的CRTF对转风扇为对象,对比分析了Heidmann模型、K-J-G模型和H-W模型对两种风扇噪声预测精度,模拟计算了飞机起飞过程中对转风扇和传统风扇的远场噪声水平。研究分析得出Heidmann模型和K-J-G模型预测CF6-80C2发动机风扇噪声数值和趋势接近,H-W模型与上述两种模型的结果在高频部分相差2~5 dB;对转风扇噪声级频谱与传统风扇在趋势上比较接近;结果表明,性能参数相似的传统风扇和对转风扇的噪声水平比较接近,对转风扇在降噪方面相对于传统风扇并没有明显优势。     

平面运动中的摩擦力

本文提出一种摩擦力和速度的连续关系式,并把非连续、非线性的方程包括在这个关系式中,解出各种情况的法向反力。     

集成锁相频率合成器设计

介绍实际应用中使用集成锁相频率合成芯片MB1504构成频率合成器的设计原理和应用方法,以实现小型化,低成本,低功耗,高品质的频率综合器。     

SAR间歇采样散射波干扰

提出一种新的合成孔径雷达（SAR）干扰方法：SAR间歇采样散射波干扰。将间歇采样转发干扰和散射波干扰结合, 实现携带真实目标散射信息的多假目标干扰。间歇采样转发干扰能实现在波形捷变SAR当前脉冲内及时转发进行对抗,而散射波干扰携带真实目标在方位向的多普勒调制散射信息。本方法将两者的优势结合,使干扰具备对抗波形捷变SAR的潜力,是一种巧妙的干扰样式。这为实现对波形捷变SAR干扰提供了一种可行的途径。仿真实验验证了该干扰方法的可行性和有效性。     

Principle of machining variant with counter curvature blending surfaces torus cutter

基于宽行加工理论和广域曲率吻合原则,提出一种利用圆环面内侧作为刀具工作面的反圆环面刀具宽行加工叶片进排气边的新方法.该方法通过优化刀具摆角使具有定母圆半径刀具工作面的包络面充分逼近叶片进排气边曲面,从而使刀具能在给定的精度范围内以最大行宽和最少刀轨行数加工出进排气边.最后,以某型号发动机叶片的进气边为例进行了加工实验.结果表明该方法能够大幅提高进排气边的加工质量,且反圆环面刀的加工行宽比球头刀提高了5倍.     

Variation of ionospheric total electron content at crest of equatorial anomaly in China from 1997 to 2004

The periodic variation of TEC data at Xiamen station (geographic coordinate: 24.4°N, 118.1°E; geomagnetic coordinate: 13.2°N, 187.4°E) at crest of equatorial anomaly in China from 1997 to 2004 is analyzed. The characteristic of TEC association with solar activity and geomagnetic activity are also analyzed. The method of continuous wavelet, cross wavelet and wavelet coherence transform methods have been used. Analysis results show that long-term variations of TEC at Xiamen station are mainly controlled by the variations of solar activities. Several remarkable components including 128–256 days, 256–512 days and 512–1024 days exist in TEC variations. The TEC data at Xiamen station is in anti-phase with geomagnetic Dst index in semiannual time-scale, but this response only exists during high solar activity. Diurnal variation of TEC is studied for different seasons. Some features like the semiannual anomaly and winter anomaly in TEC have been reported.     

The solar eclipse and its associated ionospheric TEC variations over Indian stations on January 15, 2010

An annular solar eclipse occurred over the Indian subcontinent during the afternoon hours of January 15, 2010. This event was unique in the sense that solar activity was minimum and the eclipse period coincides with the peak ionization time at the Indian equatorial and low latitudes. The number of GPS receivers situated along the path of solar eclipse were used to investigate the response of total electron content (TEC) under the influence of this solar eclipse. These GPS receivers are part of the Indian Satellite Based Augmentation System (SBAS) named as ‘GAGAN’ (GPS Aided Geo Augmented Navigation) program. The eight GPS stations located over the wide range of longitudes allows us to differentiate between the various factors induced due to solar eclipse over the equatorial and low latitude ionosphere. The effect of the eclipse was detected in diurnal variations of TEC at all the stations along the eclipse path. The solar eclipse has altered the ionospheric behavior along its path by inducing atmospheric gravity waves, localized counter-electrojet and attenuation of solar radiation intensity. These three factors primarily control the production, loss and transport of plasma over the equatorial and low latitudes. The localized counter-electrojet had inhibited the equatorial ionization anomaly (EIA) in the longitude belt of 72°E–85°E. Thus, there was a negative deviation of the order of 20–40% at the equatorial anomaly stations lying in this ‘inhibited EIA region’. The negative deviation of only 10–20% is observed for the stations lying outside the ‘inhibited EIA region’. The pre-eclipse effect in the form of early morning enhancement of TEC associated with atmospheric gravity waves was also observed during this solar eclipse. More clear and distinctive spatial and temporal variations of TEC were detected along the individual satellite passes. It is also observed that TEC starts responding to the eclipse after 30 min from start of eclipse and the delay of the maximum TEC deviation from normal trend with respect to the maximum phase of the eclipse was close to one hour in the solar eclipse path.     

舰载雷达主动反电子侦察技术

目前舰载雷达主要采用捷变频、复杂重频、宽带高增益脉冲压缩、低副瓣天线以及发射功率管控等低截获概率设计技术来提高其反电子侦察和抗干扰能力,属于“防御性”的反电子侦察技术。从电子侦察系统的特点及存在的弱点出发,提出对其进行干扰的可能性,采取主动反电子侦察的方法来掩护己方舰载雷达工作,提高舰载雷达的电子对抗能力。     

Ionospheric variation at Thailand equatorial latitude station: Comparison between observations and IRI-2001 model predictions

In this paper, the F2-layer critical frequency (foF2) and peak height (hmF2) measured by the FM/CW ionosonde at Thailand equatorial latitude station, namely Chumphon (10.72°N, 99.37°E, dip 3.22) are presented. The measurement data during low solar activity from January 2004 to December 2006 are analyzed based on the diurnal, seasonal variation. The results are then compared with IRI-2001 model predictions. Our study shows that: (1) In general, both the URSI and CCIR options of the IRI model give foF2 close to the measured ones, but the CCIR option produces a smaller range of deviation than the URSI option. The agreement during daytime is generally better than during nighttime. Overestimation mostly occurs in 2004 and 2006, while underestimation is during pre-sunrise hours in June solstice in 2005. The peak foF2 around sunset is higher during March equinox and September equinox than the other seasons, with longer duration of maximum levels in March equinox than September equinox. Large coefficients of variability foF2 occur during pre-sunrise hours. Meanwhile, the best agreement between the observed foF2 and the IRI model is obtained in June solstice. (2) In general, The IRI (CCIR) model predicts the observed hmF2 well during daytime in June solstice from 2004–2006, but it overestimates during March equinox, September equinox and December solstice. For nighttime, the model overestimates hmF2 values for all seasons especially during March equinox and September equinox. However, the model underestimates hmF2 values during September equinox and for some cases during June solstice and December solstice at pre-sunrise. The agreement between the IRI model and the hmF2(M3000_OBS) is worst around noontime, post-sunset and pre-sunrise hours. All comparative studies give feedback for new improvements of CCIR and URSI IRI models.