An algorithm to separate wind tunnel background noise from turbulent boundary layer excitation

Wall pressure fluctuations generated by Turbulent Boundary Layers(TBL) provide a significant contribution in reducing the structural vibration and the aircraft cabin noise. However,it is difficult to evaluate these fluctuations accurately through a wind tunnel test because of the pollution caused by the background noise generated by the jet or the valve of the wind tunnel. In this study, a new technology named Subsection Approaching Method(SAM) is proposed to separate the wall pressure fluctuations from the background noise induced by the jet or the valve for a transonic wind tunnel test. The SAM demonstrates good performance on separating the background noise from the total pressure compared to the other method in this study. The investigation considers the effects of the sound intensity and the decay factor on the sound-source separation. The results show that the SAM can derive wall pressure fluctuations effectively even when the level of background noise is considerably higher than the level of the wall pressure fluctuations caused by the TBL. In addition, the computational precision is also analyzed based on the broad band noise tested in the wind tunnel. Two methods to improve the precision of the computation with the SAM are also suggested: decreasing the loop gain and increasing the sensors for the signal analysis.     

远程教学在精品课程建设中的尝试

精品课程的建设实现了资源的共享,辅助了教师的教学,但精品课程的建设中存在内容不能及时更新、利用率低等问题。通过建立后台管理操作系统,管理员可方便地对内容进行补充更新的远程教学模式在精品课程中的尝试,克服了精品课程建设当中的不足,使用更加方便。     

点缀你的主页

随着因特网的发展，主页不在只是网络服务商可以做的事情，那么主页内容以及它的可观赏性就成了它吸引读者的中心。本文简述图形及动画制作方法。运用这些图形及动画来修饰主页，以启到画龙点睛的作用。     

The impact of different background errors in the assimilation of satellite radiances and in-situ observational data using WRFDA for three rainfall events over Iran

Satellite radiances and in-situ observations are assimilated through Weather Research and Forecasting Data Assimilation (WRFDA) system into Advanced Research WRF (ARW) model over Iran and its neighboring area. Domain specific background error based on x and y components of wind speed (UV) control variables is calculated for WRFDA system and some sensitivity experiments are carried out to compare the impact of global background error and the domain specific background errors, both on the precipitation and 2-m temperature forecasts over Iran. Three precipitation events that occurred over the country during January, September and October 2014 are simulated in three different experiments and the results for precipitation and 2-m temperature are verified against the verifying surface observations. Results show that using domain specific background error improves 2-m temperature and 24-h accumulated precipitation forecasts consistently, while global background error may even degrade the forecasts compared to the experiments without data assimilation. The improvement in 2-m temperature is more evident during the first forecast hours and decreases significantly as the forecast length increases.     

背景风场维持的中尺度受导重力波

提出了由上层大气背景风场所维持形成的中尺度重力波受导传播机制,通过一种新的全波解数值方法计算了这种受导波的色散关系和衰减距离。与Ｍｉｌｌｓｔｏｎｅ Ｈｉｌｌ地区 动的观测结果进行了比较,很好地解释了该地区的扰动风场滤波现象。     

武汉上空背景Na层长期变化和夜间变化特征的激光雷达观测研究

通过分析武汉大学激光雷达在2001年4月到2004年12月的观测数据,研究武汉(30.5°N,1144°E)上空背景Na层的长期(时间尺度大于1年)变化和夜间变化特征,并讨论了这种变化特征可能的产生原因.Na层长期变化的观测研究表明,背景Na层柱密度最大值出现在11月,大约是5月份最小值(1.6×109 cm-2)的2倍;质心高度最大出现在8月,比年平均高度91.5km高14km,最小值出现在5月,为91.2km;rms宽度平均值为4.5 km,最大值和最小值分别出现在12月和3月;月平均Na层质心高度和均方根宽度都具有准半年周期的变化,但两者变化的相位相反.除了长期变化外,背景Na层还呈现出明显的夜间变化特征:除凌晨短暂的时间外,Na层柱密度随夜间时间增加,于0530 LT达到最大值(2.9×109 cm-2);峰值对应的高度随时间下降;质心高度随时间缓慢增加但在凌晨迅速下降基本恢复到入夜时的高度;整夜背景Na层平均柱密度、峰值对应的高度、质心高度和rmS宽度起伏值分别为1.1×109cm-2,3 km,0.3 km和0.8 km.      

基于背景差分的动目标检测算法研究

提出一种新的基于背景差分的动目标检测算法。综合利用序列图像的时、空域信息提取目标。用中值法建立初始背景,并采用一种自适应的背景更新策略。实验结果表明,该算法简单,鲁棒性好,能够解决全局光照缓变和突变的问题,在复杂环境中也能准确地检测出运动目标。     

Relative ionizations in the nearest interstellar gas

We compare CLOUDY predictions for the equilibrium ionization in the interstellar cloud surrounding the solar system with pick-up ion data. The incident radiation field includes contributions from hot stars, the emission from the conductive cloud boundary and the diffuse FUV back-ground. To within the observational uncertainties, CLOUDY predictions for the ratios n(He)/n(O), n(N)/n(O), n(Ne)/n(O), and n(He)/n(Ne) are consistent with pick-up ion data, provided that O and N are filtered by 50% in the heliopause region and the outer heliosphere as predicted by others. Thus, the steady-state ionization model and assumed radiation field appear approximately valid. However, the youth and low intervening column density towards the Vela pulsar leave open the possibility that the parent supernova explosion 10,500 years ago, and 200 pc distant, may also have affected LISM ionization, although the mechanism is uncertain. Support for this last possibility is provided by the apparent signature of the Vela explosion in the terrestrial geological record.Abbreviations ISM Interstellar Medium - FUV Far Ultraviolet - EUV Extreme Ultraviolet - SNR SN remnant - SXRB SXR Background - LISM Local Interstellar Matter     

来流参数对混合管道流场结构的影响

为了探究来流参数对混合管道流场结构的影响,通过试验和数值计算方法研究了在不同马赫数、静压来流参数条件下的背景流场和激波串流场结构。试验采用高速纹影和压力测量设备分别进行流场的观察和测量,采用喷管支板结构将来流分为上侧二次流、一次流和下侧二次流。试验与数值结果均表明,背景流场中的背景波系、混合层均由支板后缘处产生,背景波系在壁面间反射并与混合层发生干扰作用,背景流场结构较为复杂。一、二次流的静压关系影响混合层的初始发展方向,导致θ从-9°～7°变化,而马赫数决定起始激波与混合层的夹角。依据前缘激波的反射类型、亚声速区面积等特征,混合管道的激波串流场可以分为规则反射型、临界反射型、正向马赫反射型和反向马赫反射型四种典型结构。临界反射型的波后流场在垂直流动方向上具有"亚-超-亚-超"间隔流动的特点。     

The local bubble

Recently, observations with the rosat PSPC instrument and the spectrometers onboard the euve satellite have given new detailed information on the structure and physical conditions of the Local Bubble. From the early rocket experiments, and in particular from the WISCONSIN Survey, the existence of a diffuse hot gas in the vicinity of the solar system, extending out to about 100 pc, has been inferred in order to explain the emission below 0.3 keV. The higher angular resolution and sensitivity of rosat made it possible to use diffuse neutral clouds as targets for shadowing the soft X-ray background. Thus, in some directions, more than half of the flux in the 0.25 keV band appears to come from outside the Local Bubble. Further, measurements of the diffuse EUV in the LISM, show surprisingly few emission lines. These findings are in conflict with the standard LHB model, which assumes a local hot (T 10⁶ K) plasma in CIE. Model calculations, based on the non-equilibrium cooling of an expanding plasma, show a promising way of reconciling all available observations. Thus the present temperature within the LB may be as low as 4 × 10⁴ K and its number density as large as 2 × 10^–2 cm ^–3, giving a total pressure that is roughly in agreement with the Local Cloud.Abbreviations CIE collisional ionization equilibrium - ISM Interstellar Medium - LHB Local Hot Bubble - LB Local Bubble - LISM Local ISM - SB superbubble - SXR soft X-ray - SXRB SXR Background - VLISM Very Local ISM Heisenberg Fellow