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。     

2219铝合金搅拌摩擦焊缝Al2Cu相聚集行为特征分析

对2219C10S状态铝合金进行搅拌摩擦焊接试验,发现焊缝中存在聚集物的异常聚集现象,聚集相在X光检测中显示为亮白色聚集物,主要形态分为团块状、线状和指状三种,聚集相处焊缝的力学性能与无聚集相焊缝的力学性能基本相同。各形态聚集相的分布位置受搅拌头焊接影响区域的不同而不同,团块状聚集相主要存在于焊核中心或偏焊缝上表面位置处,线状和指状聚集相主要存在于焊核中心或偏焊缝根部位置处。对异常聚集相进行能谱分析知,聚集相主要组成元素为Al和Cu,原子百分比近似为2∶1,确定聚集相主要成分为Al2Cu。对聚集相的成因进行分析认为,聚集相的产生主要受搅拌摩擦焊接热输入及搅拌头机械搅拌作用的影响,在焊接过程中,塑态软化金属中的Al2Cu在填补搅拌针后方空腔的过程中出现了聚集行为,随着塑态金属的凝固,聚集行为开始变得缓慢并结束。     

Ti/Al叠层结构低频振动制孔试验研究

钛合金与铝合金叠层构件的装配孔制备过程中存在孔壁质量差、尺寸超差等问题,为解决该问题,开展了低频轴向振动扩孔、铰孔与传统扩孔、铰孔的对比试验,重点分析了其在切屑形态、加工质量等方面的差异.结果表明,振动制孔技术能够产生C形或发条形切屑,利于切屑排出,减小铝合金孔壁的划伤.使用振动辅助技术进行一次扩孔与一次铰孔后,钛合金与铝合金孔壁粗糙度均可低于Ra0.6μm,孔径精度可满足H7公差等级,出口毛刺高度小于200μm.     

A heuristic derivation of an improved analytical theory for perpendicular diffusion of charged particles

A heuristic derivation of an improved nonlinear guiding center theory for perpendicular diffusion of charged particles is presented. This new derivation complements previous work which is based on an indirect solution of the Fokker–Planck equation. The new derivation confirms the improved theory for diffusion of charged particles and makes the validity of the theory plausible.     

Solar cycle and latitude dependence of high-beta suprathermal plasma conditions in interplanetary space between 1.3 and 5.4 AU

The analysis of energetic particles and magnetic field measurements from the Ulysses spacecraft has shown that in a series of events, the energy density contained in the suprathermal tail particle distribution is comparable to or larger than that of the magnetic field, creating conditions of high-beta plasma. In this work we analyze periods of high-beta suprathermal plasma occurrences (β_ep > 1) in interplanetary space, using the ratio (β_ep) of the energetic particle (20 keV to ∼5 MeV) and magnetic field energy densities from measurements covering the entire Ulysses mission lifetime (1990–2009) in order to reveal new or to reconfirm some recently defined interesting characteristics. The main key-results of the work are summarized as follows: (i) we verify that high-beta events are detected within well identified regions corresponding mainly to the vicinity of shock surfaces and magnetic structures, and associated with energetic particle intensity enhancements due to (a) reacceleration at shock-fronts and (b) unusually large magnetic field depressions. (ii) We define three considerable features for the high-beta events, concentrated on the next points: (a) there is an appreciable solar-activity influence on the high-beta events, during the maximum and middle solar-cycle phase, (b) the annual peak magnitude and the number of occurrences of high events are well correlated with the sunspot number, (c) the high-beta suprathermal plasma events present a spatial distribution in heliographic latitudes (HL) up to ∼±80°, and a specific important concentration on the low (−25° ? HL < −6°, 6° < HL ? 25°) and median (−45° ? HL < −25°, 25° < HL ? 45°) latitudes. We also reconfirm by a statistical analysis the results of Marhavilas and Sarris (2011), that the high-beta suprathermal plasma (β_ep > 1) events are characterized by a very large parameter β_ep (up to 1732.5), a great total duration (406 days) and a large percentage of the Ulysses-mission lifetime (which is equal to 6.34% of the total duration with usable measurements, and 11.3% of the duration in presence of suprathermal particles events).     

The hydroxyl radical as an indicator of SEP fluxes in the high-latitude terrestrial atmosphere

The low background values at nighttime of the mesospheric hydroxyl (OH) radical make it easier to single out the atmospheric response to the external solar forcing in Polar Regions. Because of the short lifetime of HO_x, it is possible to follow the trails of Solar Energetic Particle (SEP) events in the terrestrial atmosphere, as shown by Storini and Damiani (2008). The sensitivity of this indicator makes discernible not only extreme particle events with a flux peak of several thousand pfu [1 pfu = 1 particle/(cm² s sr)] at energies >10 MeV, but also those with lower flux up to about 300 pfu. Using data from the Microwave Limb Sounder (MLS) on board the EOS AURA satellite, we examined the correlation of OH abundance vs. solar proton flux for almost all the identified SEP events spanning from November 2004 to December 2006 (later on no more SEP events occurred during Solar Cycle no. 23). The channels at energies greater than 5 MeV and 10 MeV showed the best correlation values (r ∼ 0.90–0.95) at altitudes around 65–75 km whereas, as expected, the most energetic channels were most highly correlated at lower altitudes. Therefore, it is reasonably possible to estimate the solar proton flux from values of mesospheric OH (and viceversa) and it could be useful in studying periods with gaps in the records of solar particles.     

Fatigue crack propagation of new aluminum lithium alloy bonded with titanium alloy strap

A new type of aluminum lithium alloy (Al-Li alloy) Al-Li-S-4 was investigated by test in this paper. Alloy plate of 400 mm · 140 mm · 6 mm with single edge notch was made into samples bonded with Ti-6Al-4V alloy (Ti alloy) strap by FM 94 film adhesive after the surface was treated. Fatigue crack growth of samples was investigated under cyclic loading with stress ratio (R) of 0.1 and load amplitude constant. The results show that Al-Li alloy plate bonded with Ti alloy strap could retard fatigue crack propagation. Retardation effect is related with width and thickness of strap. Flaws have an observable effect on crack propagation direction.     

PDPA技术在圆管射流测量中的应用

采用激光相位多普勒技术（ＰＤＰＡ）和传统热线对圆管射流进行试验研究，试验结果表明：ＰＤＰＡ技术具有精度高、动态响应快、不干扰流场等特点；自由剪切湍流的扩展率ｄｙｃ／ｄｘ＝０．０８０１，完全自模拟特性区在ｘ／Ｄ＞８。     

What Determines the Composition of SEPs in Gradual Events?

Gradual solar energetic particle (SEP) events are evidently accelerated by coronal/interplanetary shocks driven by coronal mass ejections. This talk addresses the different factors which determine the composition of the accelerated ions. The first factor is the set of available seed populations including the solar wind core and suprathermal tail, remnant impulsive events from preceding solar flares, and remnant gradual events. The second factor is the fractionation of the seed ions by the injection process, that is, what fraction of the ions are extracted by the shock to participate in diffusive shock acceleration. Injection is a controversial topic since it depends on the detailed electromagnetic structure of the shock transition and the transport of ions in these structured fields, both of which are not well understood or determined theoretically. The third factor is fractionation during the acceleration process, due to the dependence of ion transport in the turbulent electromagnetic fields adjacent to the shock on the mass/charge ratio. Of crucial importance in the last two factors is the magnetic obliquity of the shock. The form of the proton-excited hydromagnetic wave spectrum is also important. Finally, more subtle effects on ion composition arise from the superposition of ion contributions over the time history of the shock along the observer’s magnetic flux tube, and the sequence of flux tubes sampled by the observer.