气固两相管道流中柱状粒子取向的数值研究

本文对管道悬浮流中柱状粒子的取向分布进行研究。首先对柱状粒子在流场内的运动进行数值模拟，然后运用统计方法得出大量柱状粒子的取向分布；得到了粒子长径比、St数和流场区域对粒子取向分布的影响。计算结果表明，柱状粒子长径比和St数的变化对粒子取向分布的影响并不明显，而流场区域所造成的流场横向速度梯度对粒子取向分布有重要的影响。随着流场横向速度梯度的增大，粒子有明显的占优取向，且当流场横向速度梯度增大到一定程度时，粒子取向都趋向于流动方向。文中部分结果与实验进行了比较，两者吻合较好。     

纳米锑颗粒的制备及其分散性研究

采用电化学方法电沉积制得不同形貌及粒径的纳米锑颗粒,并在制备过程中使用OP-10对纳米锑颗粒表面进行了原位改性.通过TEM、XRD、FTIR等方法对纳米锑颗粒的形态、物相和包覆效果进行表征.结果显示,纳米锑颗粒的制备具有时间效应和电流效应.随着反应时间的加长,纳米锑颗粒粒径变大,且在某种程度上存在着团聚现象;电流密度在一定范围内,适当增大电流密度有利于纳米锑颗粒的形成.纳米锑颗粒的表面改性,主要是通过OP-10的长链分子结构与纳米锑颗粒之间的化学吸附以及OP-10的长链烷基分子之间的氢键、范德华力相互作用,分子链相互缠结,部分通过C-H键互相渗入,最终有效地包覆在纳米锑颗粒表面来达到其表面改性效果,同时在反应过程中醚键也起了一定作用.纳米锑颗粒在纯液体石蜡油中的分散稳定性能与其添加量有关,其最佳添加量为0.5％.     

Simulation of ASTROD I test mass charging due to solar energetic particles and interplanetary electrons

As ASTROD I travels through space, its test mass will accrue charge due to exposure of the spacecraft to high-energy particles. This test mass charge will result in Coulomb forces between the test mass and the surrounding electrodes. In earlier work, we have used the GEANT 4 toolkit to simulate charging of the ASTROD test mass due to cosmic-ray protons of energies between 0.1 and 1000 GeV at solar maximum and at solar minimum. Here we use GEANT 4 to simulate the charging process due to solar energetic particle events and interplanetary electrons. We then estimate the test mass acceleration noise due to these fluxes. The predicted charging rates range from 2247 e⁺/s to 47,055 e⁺/s, at peak intensity, for the four largest SEP events in September and October 1989. Although the noise due to charging exceeds the ASTROD I budget for the two larger events, it can be suppressed through continuous discharging. The acceleration noise during the two small events is well below the design target. The charging rate of the ASTROD I test mass due to interplanetary electrons in this simulation is about −11% of the cosmic-ray protons at solar minimum, and over −37% at solar maximum. In addition to the Monte Carlo uncertainty, an error of ±30% in the net charging rates should be added to account for uncertainties in the spectra, physics models and geometry implementations.     

Solar energetic particle events during the rise phases of solar cycles 23 and 24

We present a comparative study of the properties of coronal mass ejections (CMEs) and flares associated with the solar energetic particle (SEP) events in the rising phases of solar cycles (SC) 23 (1996–1998) (22 events) and 24 (2009–2011) (20 events), which are associated with type II radio bursts. Based on the SEP intensity, we divided the events into three categories, i.e. weak (intensity < 1 pfu), minor (1 pfu < intensity < 10 pfu) and major (intensity ? 10 pfu) events. We used the GOES data for the minor and major SEP events and SOHO/ERNE data for the weak SEP event. We examine the correlation of SEP intensity with flare size and CME properties. We find that most of the major SEP events are associated with halo or partial halo CMEs originating close to the sun center and western-hemisphere. The fraction of halo CMEs in SC 24 is larger than the SC 23. For the minor SEP events one event in SC23 and one event in SC24 have widths < 120° and all other events are associated with halo or partial halo CMEs as in the case of major SEP events. In case of weak SEP events, majority (more than 60%) of events are associated with CME width < 120°. For both the SC the average CMEs speeds are similar. For major SEP events, average CME speeds are higher in comparison to minor and weak events. The SEP event intensity and GOES X-ray flare size are poorly correlated. During the rise phase of solar cycle 23 and 24, we find north–south asymmetry in the SEP event source locations: in cycle 23 most sources are located in the south, whereas during cycle 24 most sources are located in the north. This result is consistent with the asymmetry found with sunspot area and intense flares.     

不同形貌Ni颗粒对向列相液晶电光性能的影响

将不同形貌的Ni颗粒(类碗状Ni颗粒、Ni花颗粒和Ni球颗粒)掺杂在液晶中制备了扭曲向列相(TN)液晶显示模式液晶盒,采用液晶综合参数测试仪对掺杂不同形貌Ni颗粒的向列相液晶(NLC)显示模式液晶盒的阈值电压、饱和电压、对比度及响应时间进行了研究。结果表明,掺杂Ni颗粒后,液晶的电光性能得到明显改善,阈值电压、饱和电压均有所降低,对比度明显增大,响应时间下降。其中类碗状Ni颗粒改善效果最为明显,驱动电压降幅达到13.77%,对比度增大35.55%,响应时间降低至9.390 ms。Ni颗粒的形貌及比表面积对液晶的电光性能有很大影响。比表面积及曲率大的Ni颗粒对液晶电光性能的改善效果好。      

强驻波声场对微小颗粒群作用的实验研究

用实验手段研究了以空气为介质的强驻波声场 (声压级大于 1 5 0dB)对其中微小颗粒群 (颗粒直径小于 30 μm)的作用。实验中观察到了颗粒有规律地向波节点运动的现象 ,并发现聚集颗粒群中含有周期性长大、破裂而喷发的气泡。这些现象与声流及声辐射压力有关。对这些现象的观察和分析有助于加深对高声强下一些基本效应的认识     

高速摄像技术在循环床锅炉出口区域颗粒运动测量中的应用

为了说明高速摄像技术的一些特点 ,及其在多相流场颗粒运动规律研究方面的潜力 ,以循环床锅炉出口区域颗粒运动测量中的应用为例 ,采用高速摄像系统捕获可视化流场的图像 ,再进行图像分析和处理。通过对颗粒的运动速度、运动轨迹和密度分布等信息进行测量的结果表明 ,利用高速摄像技术能够成功地研究复杂流场的颗粒运动规律。     

Energization of charged particle in a time-dependent chaotic magnetic field with an implication of the production of seed particles in solar energetic particle events

We investigate the acceleration of charged particles in a time-dependent chaotic magnetic field in this work. In earlier works, it has been demonstrated that in an asymmetric wire-loop current systems (WLCSs), the magnetic field is of chaotic in nature. Furthermore, observations also showed that there exist time-varying current loops and current filaments in solar corona. It is therefore natural to conceive that the magnetic field on the solar surface is chaotic and time-dependent. Here, we develop a numerical model to study the acceleration process of charged particles in a time-varying chaotic magnetic field that is generated by an ensemble of 8 WLCSs. We found that the motion of energetic particles in the system is of diffusive in nature and a power law spectrum can quickly develop. The mechanism examined here may serve as an efficient pre-acceleration mechanism that generates the so-called seed particles for diffusive shock acceleration at a coronal mass ejection (CME) driven shock in large solar energetic particle (SEP) events.     

两种7050铝合金厚板的组织与性能

对两种61mm厚的7050-T7451铝合金板材进行对比分析,探讨工艺-组织-性能的关系。采用光学显微镜、扫描电镜进行组织观察,并进行室温拉伸、断裂韧性、剥落腐蚀等性能测试,实验表明:两种板材的综合性能均满足AMS 4050H标准的指标要求,但一种板材的强度、断裂韧度略低于另一种相同规格的板材,而剥落腐蚀性能略好。两种产品性能差异的主要原因在于,更系统的工艺控制使板材保持较好的组织均匀性、较小的再结晶比例,仅残留较少的小尺寸且均匀分布的Al7Cu2Fe相,基本无Al2Cu Mg相。     

Synthesis of TiNi/Ti_2Ni Composite Particles in Molten Salts

A new process of synthesizing TiNi/Ti2Ni composite particles, high temperature molten salts method, is introduced. This method uses molten salts as a reaction medium that does not take part in the chemical reaction and can be easily dissolved in rinsing water. Ac-cording this method, the composite particles were prepared in molten salts at 700 ℃-900 ℃. By means of differential scanning calo-rimetry (DSC), the reversible martensitic transformation of TiNi particles in these composite particles was confirmed.