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％.     

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。     

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     

Modeling the solar cosmic ray event of 13 December 2006 using ground level neutron monitor data

In order to understand the physics under extreme solar conditions such as those producing ground level enhancements of solar cosmic rays, it is important to use accurate and reliable models. The NM-BANGLE Model is a new cosmic ray model which couples primary solar cosmic rays at the top of the Earth’s atmosphere with the secondary ones detected at ground level by neutron monitors during GLEs. This model calculates the evolution of several GLE parameters such as the solar cosmic ray spectrum, anisotropy and particle flux distribution, revealing crucial information on the energetic particle propagation and distribution. The total output of the NM-BANGLE Model is a multi-dimensional GLE picture that gives an important contribution to revealing the characteristics of solar energetic particle events recorded at ground level. In this work, the results of the NM-BANGLE Model application to the recent GLE of 13 December 2006 are presented and discussed. Moreover, a comparison with the extreme event of 20 January 2005 (GLE69) has been realized.     

Ion production and ionization effect in the atmosphere during the Bastille day GLE 59 due to high energy SEPs

The influence of high energy particles, specifically cosmic rays, on atmospheric physics and chemistry is highly discussed. In most of the proposed models the role of ionization in the atmosphere due to cosmic rays is not negligible. Moreover, effect(s) on minor constituents and aerosols are recently observed, specifically over the polar regions during strong solar particle events. According to the recent findings for such effects it is necessary an essential increase of ion production, specifically during the winter period. The galactic cosmic rays are the main source of ionization in the Earth’s stratosphere and troposphere. Occasionally, the atmospheric ionization is significantly enhanced during strong solar energetic particles events, specifically over the polar caps. During the solar cycle 23 several strong ground level enhancements were observed. One of the strongest was the Bastille day event occurred on 14 July 2000. Using a full Monte Carlo 3-D model, we compute the atmospheric ionization, considering explicitly the contribution of cosmic rays with galactic and solar origin, focusing on high energy particles. The model is based on atmospheric cascade simulation with the PLANETOCOSMICS code. The ion production rate is computed as a function of the altitude above the sea level. The ion production rate is computed on a step ranging from 10 to 30?min throughout the event, considering explicitly the spectral and angular characteristics of the high energy part of solar protons as well as their time evolution. The corresponding event averaged ionization effect relative to the average due to galactic cosmic rays is computed in lower stratosphere and upper troposphere at various altitudes, namely 20?km, 15?km, 12?km and 8?km above the sea level in a sub-polar and polar regions. The 24^h and the weekly ionization effects are also computed in the troposphere and low stratosphere. Several applications are discussed.     

双补燃室固冲凝聚相颗粒分布对比试验研究

针对固冲发动机燃烧效率较低以及凝相粒子分布规律不清楚的现状,本文建立了一套评价固冲发动机燃烧效率的双补燃室试验装置和研究凝相颗粒分布的取样装置。对比研究了结构相同的补燃室内的参数,其误差小于0.5%,说明该装置可以用于精确对比不同补燃室的燃烧效率。然后应用该装置完成了补燃室长度分别为600mm、800mm、1000mm,进气角度分别为30°、45°、60°的对比试验,分析了粒子的粒度分布规律和化学成分变化规律,该规律与数值分析的规律相同。试验结果表明：在进气角度不变情况下,补燃室长度增加有利于提高燃烧效率,燃烧室压强提高,凝相粒子直径明显减小,B粒子燃烧更充分;在补燃室长度为1000mm的情况下,进气角度增加有利于燃烧效率增加,燃烧室压强提高,粒子直径减小,B粒子燃烧更充分。双补燃室发动机是评价补燃室燃烧效率的有效装置,粒度分布和燃烧产物的化学成分有助于补燃室结构设计。     

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。      

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.     

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.     

Evidence for a Two-Stage Acceleration Process in Large Solar Energetic Particle Events

Using high-resolution mass spectrometers on board the Advanced Composition Explorer (ACE), we surveyed the event-averaged ∼0.1–60 MeV/nuc heavy ion elemental composition in 64 large solar energetic particle (LSEP) events of cycle 23. Our results show the following: (1) The Fe/O ratio decreases with increasing energy up to ∼10 MeV/nuc in ∼92% of the events and up to ∼60 MeV/nuc in ∼64% of the events. (2) The rare isotope ³He is greatly enhanced over the corona or the solar wind values in 46% of the events. (3) The heavy ion abundances are not systematically organized by the ion’s M/Q ratio when compared with the solar wind values. (4) Heavy ion abundances from C–Fe exhibit systematic M/Q-dependent enhancements that are remarkably similar to those seen in ³He-rich SEP events and CME-driven interplanetary (IP) shock events. Taken together, these results confirm the role of shocks in energizing particles up to ∼60 MeV/nuc in the majority of large SEP events of cycle 23, but also show that the seed population is not dominated by ions originating from the ambient corona or the thermal solar wind, as previously believed. Rather, it appears that the source material for CME-associated large SEP events originates predominantly from a suprathermal population with a heavy ion enrichment pattern that is organized according to the ion’s mass-per-charge ratio. These new results indicate that current LSEP models must include the routine production of this dynamic suprathermal seed population as a critical pre-cursor to the CME shock acceleration process.