The dust content of clusters of galaxies

We have statistically investigated the infrared luminosity of clusters of galaxies in comparison with the known tracers of the cluster mass like the X-ray luminosity and the cluster richness (e.g. the number of member galaxies). Our results show that there is a clear positive correlation of the infrared luminosity with the cluster mass. Quantitatively speaking, the infrared luminosity is on average 20 times higher than the X-ray luminosity. Moreover, the infrared luminosity increases with the redshift. This probably shows that a major part of this infrared luminosity is due to star formation in the member galaxies. Another possible contribution would be the thermal emission from dust particles in the diffuse intracluster medium. However our method does not allow us to infer conclusions about this second hypothesis. Depending on their size and abundance, such particles would contribute to the infrared luminosity of galaxy cluster and have an impact on the cooling function of the baryons and thus on the formation of the large scale structures. This is an important cosmological question which still remains open.     

Reminiscences of cosmic ray research in Mexico

Cosmic ray research in Mexico dates from the early 1930s with the work of the pioneering physicist, Manuel Sandoval Vallarta and his students from Mexico. Several experiments of international significance were carried out during that period in Mexico: they dealt with the geomagnetic latitude effect, the north–south and west–east asymmetry of cosmic ray intensity, and the sign of the charge of cosmic rays. The international cosmic ray community has met twice in Mexico for the International Cosmic Ray Conferences (ICRC): the fourth was held in Guanajuato in 1955, and the 30th took place in Mérida, in 2007. In addition, an international meeting on the Pierre Auger Collaboration was held in Morelia in 1999, and the International Workshop on Observing UHE Cosmic Rays took place in Metepec in 2000. A wide range of research topics has been developed, from low-energy Solar Energetic Particles (SEP) to the UHE. Instrumentation has evolved since the early 1950s, from a Simpson type neutron monitor installed in Mexico City (2300 m asl) to a solar neutron telescope and an EAS Cherenkov array, (within the framework of the Auger International Collaboration), both at present operating on Mt. Sierra La Negra in the state of Puebla (4580 m asl). Research collaboration has been undertaken with many countries; in particular, the long-term collaboration with Russian scientists has been very fruitful.     

泵间管气液两相流压力波传播速度数值研究

采用ANSYS CFX热相变模型数值模拟了泵间管气氧和液氧的混合冷凝过程.并应用整体平均两流体模型建立了气液两相流压力波的色散方程,系统研究了泵间管两相压力波的传播速度特性.计算表明:泵间管气液两相波速随空泡份额的增加先减小而后在弹状流区域略微增大,且两相波速随扰动角频率增加而增大.增加液氧流量或降低进口气氧温度,气液的冷凝效果增强,沿管流的空泡份额减小,气液两相波速增大.      

基于KZK方程的声爆频域预测法

建立了一种快速预测声爆传播特性的频域方法,基于传统Khohklov-Zabolotskaya-Kuznetsov (KZK)方程,描述声爆沿激波波阵面法线方向的传播。为了验证模型正确性,以NASA TD N-161中试件C为对象,首先基于不同网格,利用计算流体力学(CFD)方法得到超音速流场;将CFD结果作傅立叶变换后代入模型方程,快速求解声爆传播特性。预测结果与NASA实验结果符合很好,研究表明：预测方法能够捕捉声爆的非线性传播,声衍射项使得声场在远场趋于轴对称分布,远距离传播后声能量集中于低频分量。     

固体中脉冲超声波传播的有限差分模拟

脉冲超声波传播过程的模拟研究对实际超声检测的信号分析具有重要的借鉴意义。对弹性固体中的声场方程应用时域有限差分法,进行了二维声场特性研究。通过完全匹配层方法对截断边界的吸收处理,解决了无限自由空间的计算问题。模拟计算表明该方法可用于各向异性介质的分析。分析了液固耦合情况下的超声波传播特性,取得了与光弹法物理试验相一致的结果。通过与平底孔试块实际缺陷回波信号的对比,验证了脉冲超声波有限差分法模拟计算的有效性和正确性。     

基于Khokhlov-Zabolotskaya-Kuznetsov方程的声爆频域预测法

建立了一种快速预测声爆传播特性的频域方法,基于传统Khokhlov-Zabolotskaya-Kuznetsov(KZK)方程,描述声爆沿激波波阵面法线方向的传播.为了验证模型正确性,以NASA TD N-161中试件C为对象,首先基于不同网格,利用计算流体动力学(CFD)方法得到超声速流场;将CFD结果作傅里叶变换后代入模型方程,快速求解声爆传播特性.预测结果与NASA实验结果符合很好,研究表明:预测方法能够捕捉声爆的非线性传播,声衍射项使得声场在远场趋于轴对称分布,远距离传播后声能量集中于低频分量.      

Evaluation of mixed mode-I/II criteria for fatigue crack propagation using experiments and modeling

In this study, in-plane mixed mode-I/II fatigue crack growth simulations and experiments are performed for the Al 7075-T651 aluminum alloy which is widely used in the aerospace industry. Tests are carried out under different mode mixity ratios to evaluate the applicability of a fracture criterion developed in a previous study to mixed mode-I/II fatigue crack growth tests. Results obtained from the analyses and experiments are compared with existing and developed criteria in terms of crack growth lives. Compact Tension Shear (CTS) specimens, which enable mixed mode loading with loading devices under different loading angles, are used in the simulations and experiments. In an effort to model and simulate the actual conditions in the experiments, crack surfaces of fractured specimens are scanned, crack paths are modeled exactly, and contacts are defined between the contact surfaces of a specimen and the loading device for each crack propagation step in the analyses. Having computed the mixed mode stress intensity factors from the numerical analyses, propagation life cycles are predicted by existing and the developed mixed mode-I/II criteria and then compared with experimental results.     

Fast solar radiation pressure modelling with ray tracing and multiple reflections

Physics based SRP (Solar Radiation Pressure) models using ray tracing methods are powerful tools when modelling the forces on complex real world space vehicles. Currently high resolution (1?mm) ray tracing with secondary intersections is done on high performance computers at UCL (University College London). This study introduces the BVH (Bounding Volume Hierarchy) into the ray tracing approach for physics based SRP modelling and makes it possible to run high resolution analysis on personal computers. The ray tracer is both general and efficient enough to cope with the complex shape of satellites and multiple reflections (three or more, with no upper limit). In this study, the traditional ray tracing technique is introduced in the first place and then the BVH is integrated into the ray tracing. Four aspects of the ray tracer were tested for investigating the performance including runtime, accuracy, the effects of multiple reflections and the effects of pixel array resolution.Test results in runtime on GPS IIR and Galileo IOV (In Orbit Validation) satellites show that the BVH can make the force model computation 30–50 times faster. The ray tracer has an absolute accuracy of several nanonewtons by comparing the test results for spheres and planes with the analytical computations. The multiple reflection effects are investigated both in the intersection number and acceleration on GPS IIR, Galileo IOV and Sentinel-1 spacecraft. Considering the number of intersections, the 3rd reflection can capture $99.12\%\text{,}99.14\%$, and $91.34\%$ of the total reflections for GPS IIR, Galileo IOV satellite bus and the Sentinel-1 spacecraft respectively. In terms of the multiple reflection effects on the acceleration, the secondary reflection effect for Galileo IOV satellite and Sentinel-1 can reach 0.2?$\text{nm}/{\text{s}}^2$ and 0.4?$\text{nm}/{\text{s}}^2$ respectively. The error percentage in the accelerations magnitude results show that the 3rd reflection should be considered in order to make it less than $0.035\%$. The pixel array resolution tests show that the dimensions of the components have to be considered when choosing the spacing of the pixel in order not to miss some components of the satellite in ray tracing. This paper presents the first systematic and quantitative study of the secondary and higher order intersection effects. It shows conclusively the effect is non-negligible for certain classes of misson.     

飞机表面绕射射线的寻迹方法

研究一种电子对抗特种飞机表面绕射射线的寻迹新方法.对飞机进行快速三维几何建模和表面网格剖分,并根据需要对几何模型的剖面和结点加密,生成飞机表面网格数据;选定寻迹区域,对飞机表面网格结点进行管理,根据费马原理,采用改进的动态规划方法,在飞机表面网格上快速、准确地实现任意源点和绕射接收点间的短程线计算;在此基础上,采用递归方法实现可视化的几何绕射理论(GTD)、一致性几何绕射理论(UTD)绕射射线离散寻迹.绕射射线离散寻迹为数值方法求解机身表面任意两点间的天线隔离度提供了条件.      

New results on the time histories of gamma-ray bursts

A study of the morphology of 14 short ( 1 s) gamma ray bursts observed by the Franco Soviet SIGNE detectors onboard the VENERA spacecraft between 1978 and 1982 is presented. We find two major groups of short bursts characterised not only by their different durations ( 1 s and 100 ms respectively), but also by different e-folding rise and decay times. A study of the time history of the impulsive portion of the 1979 March 5 event at 2 ms resolution shows evidence for a previously undiscovered 23ms quasi periodicity. These results are discussed in the context of neutron star models for gamma ray bursters.