Y形构形微通道流动换热特性的数值分析

针对矩形芯片提出了Y形构形微通道的芯片内部冷却结构,通过三维数值计算比较了Y形构形微通道与传统直微通道中的流体层流流动和换热特性,并对Y形构形微通道的重要结构参数进行了优化.研究表明:在相同对流换热面积和水利直径的条件下,Y形构形微通道具有比直微通道更高的传热效率和更低的进出口压降,可以满足高热负荷需求.在研究范围内通道级数为3级、分叉角度为60°、分支个数为2时,散热器的综合换热性能最好.以上结论为Y形构形微通道的结构设计提供了重要依据.     

网格式肋化通道换热与总压损失特性研究

通过两个实验模型,对矩形网格式肋化通道的换热与总压损失特性进行了实验研究。模型通道的两个宽边是由铝板机械加工而成的肋化壁,两个短边是由胶木板制成的绝热壁。肋化壁上肋与通道轴线所形成的锐角定义为肋向角α,第一个模型的两个宽边上的肋向角分别为45°和-45°(简称45/45模型);第二个模型两宽边的肋向角分别为45°和-60°(简称45/60模型)。两个模型的肋宽与肋间距之比t/p=0.25,肋间距与肋高之比t/e=0.30,肋高与通道高度之比e/H=0.50,即两个肋化壁的肋尖相互接触,从而形成网格式通道。实验表明当雷诺数在0.5×105～1.2×105范围内变化时,网格式内冷通道换热效果比光滑通道提高了5～9倍,但伴随的总压损失增加了3个数量级。      

超声速尾迹-剪切流的混合增强

超声速条件下燃料和空气之间的高效混合是超然冲压发动机技术上的主要挑战。基于大涡模拟和流动稳定性分析,针对超声速尾迹-剪切流动开展了混合增强方法研究。尾迹的存在改变了混合层流动的速度剖面,对流动稳定性产生了重要影响,使混合层由三维最不稳定变为二维最不稳定,最不稳定扰动波频率和增长率增大。基于流动稳定性结果引入扰动的混合增强方式依然有效,根据稳定性结果设计了波纹隔板。数值结果表明：二维波纹壁引入的扰动未能增长,不具备混合强化效果,而三维波纹壁引入的扰动能够快速增长,具有混合强化效果,且波纹壁参数越接近最不稳定扰动波参数,混合强化效果越明显。     

被动型星载氢钟H型气体电离模型及参数优化

针对被动型星载氢钟气体电离装置低功耗、低电磁干扰的设计要求,设计了一种基于平面盘绕馈能天线的H型电离系统,并建立该电离方法的数学模型。首先,由Maxwell方程出发,推导出了电离泡中的电场和磁场的分布模型,得到气体电离机制;再由电磁场的分布方程推导出氢气击穿判据表达式,建立了气体电离条件的数学模型;最后,利用电离击穿条件判据方程优化了电离装置的设计参数。数值仿真与测试表明该模型是有效的,采用优化的设计参数可以使电离功耗和电磁干扰特性得到改善,且电离直流电源总功率可小于2W。     

HMX炸药特性的密度泛函理论

应用密度泛函理论(DFT)的B3LYP方法,在6-31G(d)和6-31++G(d)基组水平上对HMX炸药进行了研究,计算得到了中性分子和离子的稳定构型,并确定了分子的电离能。通过对HMX红外振动光谱的理论计算和研究,发现振动光谱主要分布在I(0~1 750 cm-1)和II(3 000~3 250 cm-1)两个区域,且整个红外光谱中振动峰的实际数目远小于简正振动的数目。此外,与中性分子的红外光谱相比,HMX+的谱线强度整体要大于HMX分子的谱线强度,且最强峰和次强峰与中性分子相比出现了明显的红移。     

倾斜微槽道热管中纳米流体的应用

为了研究热管倾斜角度和压力对热管蒸发段、冷凝段传热系数以及最大换热功率的影响,对使用水基CuO纳米流体为工质的倾斜微槽道热管强化换热特性进行实验研究.实验装置主要由带角度调节功能的微槽道热管和加热、冷却系统组成.实验结果发现,用水基纳米流体替代去离子水为工质时,热管整体换热特性得到明显增强,蒸发段、冷凝段传热系数以及最大功率都能大幅度提高,总热阻明显降低.倾斜水热管的蒸发段和冷凝段传热系数比水平水热管的有大幅提高,但最大功率变化不大.而倾斜纳米流体热管不但蒸发段和冷凝段传热系数比水平纳米流体热管有大幅提高,而且最大功率更有接近一倍的增加.对水和纳米流体两种工质,对应于最佳换热特性的倾斜角都是75°.因此,纳米流体对倾斜热管有良好的应用前景.      

Temporal and spatial variation of equatorial ionization anomaly by using multistation ionosonde data for the 19th solar cycle over the Indian region

The paper deals with the study of temporal and spatial variation of equatorial ionization anomaly (EIA) phenomenon along with its dependence on solar activity and season during the 19th solar cycle by using seven Indian ionosonde stations. Present study is an attempt to carry out the comprehensive study of EIA by using the limited number of ground based instruments. This has been achieved by performing the Gaussian fitting over the latitudinal distribution of F2-region critical frequency (foF2) data. Results reveal that the phenomenon of EIA has a strong dependence on solar activity and seasons. The EIA crest exhibits the feature of latitudinal shifting and expansion with increasing solar activity. It is found out that the effect of solar cycle and seasons on EIA is local time dependent. The observations were also compared with the IRI-2001 model predictions and results reveal that the model values are in general agreement with the observed values with some discrepancies, particularly during the high solar activity period and morning sector. The results have been discussed in the light of relative contribution from transequatorial interhemispheric neutral wind and strength of equatorial fountain process during different local time, season and solar activity levels. Furthermore, an attempt is made to parameterize the location and foF2 of the EIA crest by using the regression analysis. These results can be used to predict the latitudinal position and foF2 of the EIA crest for any given 12-month running average sunspot number (R12).     

基于灰度级分组的X光行李图像增强改进方法

针对低对比度X光手提行李图像在机场安检中容易产生高虚警或高漏警的问题,提出了一种基于灰度级分组的X光行李图像增强改进方法。首先应用离散小波变换对低、高能图像进行融合,然后通过分频处理得到低、高频图像,再分别采用基本灰度级分组和可选择灰度级分组方法实现增强。将本文方法与基于灰度级分组的增强方法、传统的直方图均衡方法进行比较,实验结果表明,本文方法能够有效地改善图像质量,提高图像的清晰度。     

Normalized ionization yield function for various nuclei obtained with full Monte Carlo simulations

Several recent results important for production of ion pairs in the Earth atmosphere by various primary cosmic ray nuclei are presented. The direct ionization by various primary cosmic ray nuclei is explicitly obtained. The longitudinal profile of atmospheric cascades is sensitive to the energy and mass (charge) of the primary particle. In this study different cosmic ray nuclei are considered as primaries, namely Helium, Oxygen and Iron nuclei. The cosmic ray induced ionization is obtained on the basis of CORSIKA 6.52 code simulations using FLUKA 2006 and QGSJET II hadronic interaction models. The energy of the primary particles is normalized to GeV per nucleon. In addition, the ionization yield function Y is normalized as ion pair production per nucleon. The obtained ionization yield functions Y for various primaries are compared. The presented results and their application are discussed.     

Ionization effect of solar protons in the Earth atmosphere – Case study of the 20 January 2005 SEP event

The cosmic ray ground level enhancement on January 20, 2005 is among the largest recorded events in the history of cosmic ray measurements. The solar protons of MeV energies cause an excess of ionization in the atmosphere, specifically over polar caps following major solar disturbances. The ionization effect in the Earth atmosphere is obtained for various latitudes on the basis of solar proton energy spectra, reconstructed from GOES 11 measurements and subsequent full Monte Carlo simulation of cosmic ray induced atmospheric cascade. The estimation of ionization rates is based on a numerical model for cosmic ray induced ionization. The evolution of atmospheric cascade is performed with the CORSIKA 6.52 code using FLUKA 2006b and QGSJET II hadron interaction models. The atmospheric ion rate ionization is explicitly obtained for 40°N, 60°N and 80°N latitudes. The time evolution of obtained ion rates is presented. It is demonstrated that ionization effect is negative for 40°N and small for 60°N, because of accompanying Forbush decrease. The ionization effect is significant only in sub-polar and polar atmosphere during the major ground level enhancement of 20 January 2005.