Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.     

Fe/O Ratios in Interplanetary Shock Accelerated Particles

It is widely accepted that diffusive shock acceleration is an important process in the heliosphere, in particular in producing the energetic particles associated with interplanetary shocks driven by coronal mass ejections. In its simplest formulation shock acceleration is expected to accelerate ions with higher mass to charge ratios less efficiently than those with lower mass to charge. Thus it is anticipated that the Fe/O ratio in shock-accelerated ion populations will decrease with increasing energy above some energy. We examine the circumstances of five interplanetary shocks that have been reported to have associated populations in which Fe/O increases with increasing energy. In each event, the situation is complex, with particle contributions from other sources in addition to the shock. Furthermore, we show that the Fe/O ratio in shock-accelerated ions can decrease even when the shock is traveling through an Fe-rich ambient ion population. Thus, although shock acceleration of an Fe-rich suprathermal population has been proposed to explain large Fe-rich solar particle events, we find no support for this proposal in these observations.     

小型回流燃烧室多工况碳黑分布预测

为了研究小型回流燃烧室不同条件下的工作状态,并分析其产生积碳现象的原因,采用k-ε湍流模型、EDC湍流燃烧等模型对该燃烧室多个工况进行数值计算。结果表明,燃烧室性能参数计算值与台架数据较吻合,各个状态下参数相对误差均小于1.37%。根据各工况的温度分布的变化,发现燃烧室火焰随工况降低逐渐向火焰筒头部收缩。计算了各工况蒸发管内的燃油蒸发率,发现蒸发率在低工况时明显降低。根据出口温度分布情况,计算出口温度分布系数OTDF为0.35。分析碳黑粒子的分布,发现积碳现象主要在火焰筒头部,其原因主要是燃烧不充分和冷却气膜的缺失。     

超声速PIV示踪粒子布撒技术研究

介绍了上海交通大学高超声速创新技术研究实验室为发展超声速PIV流场测试系统而开发的示踪粒子布撒技术。研究中设计了一套超声速风洞PIV示踪粒子布撒装置,提出了利用发生器罐体内的真空度吸入示踪粒子的加注方式,选定了测试流程时序并得到了较好的粒子布撒效果。通过比较不同的发生器罐注入压力对粒子布撒浓度的影响,得到了效果良好的测试方案。     

含SiO2,ZrO2微粒复合镀镍层抗高温氧化性能

通过对含有SiO₂,ZrO₂微粒复合电沉积的研究,在Cu合金表面分别获得了含量(原子数分数)为11.3％ SiO₂,5.31％ ZrO₂微粒的Ni基复合镀层.通过在800℃、900℃条件下的高温氧化和热震循环试验,研究了这种复合镀镍层的高温氧化性能和界面结合特性.结果表明:经过40?h的高温氧化,2种复合镀镍层的抗氧化性能均达到抗氧化级,而且含SiO₂微粒的复合镀镍层的抗氧化性能优于含ZrO₂微粒的复合镀镍层;经过55次冷热循环,含SiO₂微粒的复合镀镍层与铜基体结合良好.     

Non-Thermal Processes in Cosmological Simulations

Non-thermal components are key ingredients for understanding clusters of galaxies. In the hierarchical model of structure formation, shocks and large-scale turbulence are unavoidable in the cluster formation processes. Understanding the amplification and evolution of the magnetic field in galaxy clusters is necessary for modelling both the heat transport and the dissipative processes in the hot intra-cluster plasma. The acceleration, transport and interactions of non-thermal energetic particles are essential for modelling the observed emissions. Therefore, the inclusion of the non-thermal components will be mandatory for simulating accurately the global dynamical processes in clusters. In this review, we summarise the results obtained with the simulations of the formation of galaxy clusters which address the issues of shocks, magnetic field, cosmic ray particles and turbulence.     

质子引发的单粒子翻转率估算的研究

根据质子单粒子翻转事件的物理本质,及空间高能质子环境特性,给出了一种基于重离子单粒子翻转实验数据基础之上的估算质子引发的单粒子翻转的方法.利用这种方法计算了几种器件的翻转情况,与地面模拟实验及飞行观测结果符合得非常好.      

高速流动中PIV示踪粒子松弛特性研究

示踪粒子的随流能力是PIV技术在高速流动中应用的关键点之一。在上海交通大学变马赫数高速风洞中开展了PIV实验研究,重点提出一种评价示踪粒子随流能力的松弛特性分析模型。在马赫数4条件下尖锥、尖劈等模型PIV实验研究中,可以准确分析粒子的松弛特性,粒径分析结果与实验吻合较好,并验证了高速流动PIv的测试精度和示踪粒子布撒能力。     

IMF connection for energetic protons observed at Ulysses via mid-latitude solar wind rarefaction regions

As Ulysses moved inward and southward from mid-1992 to early 1994 we noticed the occasional occurrence of inter-events, lasting about 10 days and falling between the recurrent events, observed at proton energies of 0.48–97 MeV, associated with Corotating Interaction Regions (CIR). These inter-events were present for several sequences of two or more solar rotations at intensity levels around 1% of those of the neighbouring main events. When we compared the Ulysses events with those measured on IMP-8 at 1 AU we saw that the inter-events appeared at Ulysses after the extended emission (>10 days) of large fluxes of solar protons of the same energy that lasted at least one solar rotation at 1 AU. The inter-events fell completely within the rarefaction regions (dv/dt<0) of the recurrent solar wind streams. The interplanetary magnetic field (IMF) lines in the rarefactions map back to the narrow range of longitudes at the Sun which mark the eastern edge of the source region of the high speed stream. Thus the inter-events are propagating at mid-latitudes to Ulysses along field lines free from stream-stream interactions. They are seen in the 0.39–1.28 MeV/nucleon He, which exhibit a faster decay, but almost never in the 38–53 keV electrons. We show that the inter-events are unlikely to be accelerated by reverse shocks associated with the CIRs and that they are more likely to be accelerated by sequences of solar events and transported along the IMF in the rarefactions of the solar wind streams.     

基于复杂型面薄壁零件成形的电铸试验研究

 在航空、航天领域存在诸如风洞喷管、波导元件和叶片电极等异型薄壁零件,采用常规加工方法对这些薄壁零件进行加工时存在着难加工的问题,利用一种新型的电铸技术——阴极平动式游离粒子辅助磨擦电铸技术对其进行直接成形加工。在电铸过程中,阴阳极之间添加不导电的游离粒子,随着阴极的不断运动,游离粒子能够周期性地对电沉积层产生磨擦、抛光、挤压作用,以此来提高表面质量,强化电铸层。与传统电铸技术所制备的电铸镍层进行了对比试验,试验结果表明：游离粒子辅助磨擦电铸技术能够获得表面光亮、平整电铸层;电铸层（200）晶面的衍射强度明显降低,（111）和（220）晶面的衍射强度显著提高;电铸层的机械性能也得到了明显的改善,显微硬度和抗拉强度比传统电铸工艺提高了一倍左右。以此为基础,成功制备了复杂型面叶片阴极,其显微硬度和表面粗糙度都得到了明显改善。