Galactic Wind: Mass Fractionation and Cosmic Ray Acceleration

The dynamical and chemical effects of the Galactic Wind are discussed. This wind is primarily driven by the pressure gradient of the Cosmic Rays. Assuming the latter to be accelerated in the Supernova Remnants of the disk which at the same time produce the Hot Interstellar Medium, it is argued that the gas removed by the wind is enriched in the nucleosynthesis products of Supernova explosions. Therefore the moderate mass loss through this wind should still be able to remove a substantial amount of metals, opening the way for stars to produce more metals than observed in the disk, by e.g. assuming a Salpeter-type stellar initial mass function beyond a few Solar masses. The wind also allows a global, physically appealing interpretation of Cosmic Ray propagation and escape from the Galaxy. In addition the spiral structure of the disk induces periodic pressure waves in the expanding wind that become a sawtooth shock wave train at large distances which can re-accelerate “knee” particles coming from the disk sources. This new Galactic Cosmic Ray component can reach energies of a few×10¹⁸ eV and may contribute to the juncture between the particles of Galactic and extragalactic origin in the observed overall Cosmic Ray spectrum.     

Solar and Solar-Wind Composition Results from the Genesis Mission

The Genesis mission returned samples of solar wind to Earth in September 2004 for ground-based analyses of solar-wind composition, particularly for isotope ratios. Substrates, consisting mostly of high-purity semiconductor materials, were exposed to the solar wind at L1 from December 2001 to April 2004. In addition to a bulk sample of the solar wind, separate samples of coronal hole (CH), interstream (IS), and coronal mass ejection material were obtained. Although many substrates were broken upon landing due to the failure to deploy the parachute, a number of results have been obtained, and most of the primary science objectives will likely be met. These objectives include He, Ne, Ar, Kr, and Xe isotope ratios in the bulk solar wind and in different solar-wind regimes, and ¹⁵N/¹⁴N and ¹⁸O/¹⁷O/¹⁶O to high precision. The greatest successes to date have been with the noble gases. Light noble gases from bulk solar wind and separate solar-wind regime samples have now been analyzed. Helium results show clear evidence of isotopic fractionation between CH and IS samples, consistent with simplistic Coulomb drag theory predictions of fractionation between the photosphere and different solar-wind regimes, though fractionation by wave heating is also a possible explanation. Neon results from closed system stepped etching of bulk metallic glass have revealed the nature of isotopic fractionation as a function of depth, which in lunar samples have for years deceptively suggested the presence of an additional, energetic component in solar wind trapped in lunar grains and meteorites. Isotope ratios of the heavy noble gases, nitrogen, and oxygen are in the process of being measured.     

The Origin of Mercury’s Internal Magnetic Field

Mariner 10 measurements proved the existence of a large-scale internal magnetic field on Mercury. The observed field amplitude, however, is too weak to be compatible with typical convective planetary dynamos. The Lorentz force based on an extrapolation of Mariner 10 data to the dynamo region is 10⁻⁴ times smaller than the Coriolis force. This is at odds with the idea that planetary dynamos are thought to work in the so-called magnetostrophic regime, where Coriolis force and Lorentz force should be of comparable magnitude. Recent convective dynamo simulations reviewed here seem to resolve this caveat. We show that the available convective power indeed suffices to drive a magnetostrophic dynamo even when the heat flow though Mercury’s core–mantle boundary is subadiabatic, as suggested by thermal evolution models. Two possible causes are analyzed that could explain why the observations do not reflect a stronger internal field. First, toroidal magnetic fields can be strong but are confined to the conductive core, and second, the observations do not resolve potentially strong small-scale contributions. We review different dynamo simulations that promote either or both effects by (1) strongly driving convection, (2) assuming a particularly small inner core, or (3) assuming a very large inner core. These models still fall somewhat short of explaining the low amplitude of Mariner 10 observations, but the incorporation of an additional effect helps to reach this goal: The subadiabatic heat flow through Mercury’s core–mantle boundary may cause the outer part of the core to be stably stratified, which would largely exclude convective motions in this region. The magnetic field, which is small scale, strong, and very time dependent in the lower convective part of the core, must diffuse through the stagnant layer. Here, the electromagnetic skin effect filters out the more rapidly varying high-order contributions and mainly leaves behind the weaker and slower varying dipole and quadrupole components (Christensen in Nature 444:1056–1058, 2006). Messenger and BepiColombo data will allow us to discriminate between the various models in terms of the magnetic fields spatial structure, its degree of axisymmetry, and its secular variation.     

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.     

双肋式微型气动阀的数值计算与实验

 针对现有微型三角阀效率低的问题,提出双肋式气动阀这一新型微阀,通过两级带圆弧过渡的收敛形肋条,在减小正向气流压力损失的同时,引导逆向气流分为3股后再呈“Y”形汇聚,产生强烈的相互撞击而抵消部分动能,从而减小逆向流量以提高效率。通过数值计算对双肋式气动阀的作用原理进行了分析与验证;加工了特征尺寸为1 mm的三角阀、梯形阀与双肋阀实验件,并设计了相应的实验方案,在微流体实验平台上进行了对比实验。结果表明双肋阀能大幅提高效率：对不可压流,双肋阀可将效率从普通阀的2%～3%提升至14%左右;对可压流,双肋阀能将效率从2%提升至约13%。     

穿越微下冲气流的飞翼布局无人机控制方法

微下冲气流是最危险的低空风切变形式,为在起降阶段安全穿越该气流,飞翼布局的无人机控制律应具有快速响应能力和良好的鲁棒性。针对大展弦比飞翼布局无人机舵面附加升力大和低速状态俯仰操纵效能低的特点,提出了舵面附加升力和机体气动力相结合的复合控制方案,改进了以输出误差为参考量的非线性指令分配策略,设计了基于迎角保护的指令分配策略。将风干扰和模型的不确定性视为未知扰动,采用自抗扰控制(ADRC)理论设计飞翼布局无人机非线性控制律,使之对风干扰和模型的不确定性进行估计补偿。仿真结果表明,复合控制与ADRC相结合的方法加速了航迹倾角的单位阶跃响应速度,使上升时间缩短了64%,同时能够实现对风干扰的有效观测和补偿,使高度损失低于2m;能够在风切变中有效保护迎角,使其维持在5.5°以内。因此,该方法能够为飞翼布局无人机安全平稳地穿越微下冲气流提供一种参考方案。     

高温磁悬浮轴承用位移传感器的研究

针对差动变压器式位移传感器的性能及其在高温磁悬浮轴承中的应用,对环境温度升高影响差动变压器式位移传感器（DTDS）性能的机理和特征以及所采用的温度补偿技术进行了研究。采用比值方式的处理电路以及加入补偿电阻的方法改善了温度升高所带来位移传感器灵敏度升高、温度漂移和时间漂移的问题。对不同温度下的差动变压器式位移传感器进行标定得到了位移传感器的动静态性能,并将其应用到单自由度高温磁悬浮轴承（HTAMB）试验台上进行静态和模拟动态悬浮。研究结果表明,环境温度为550 ℃,被测物体移动范围在-0.35~+0.35 mm时,位移传感器的灵敏度在19.62 mV/μm,线性度为±0.74%,迟滞性为±0.40%,重复性为±0.97%,传感器截止频率在800 Hz左右;在单自由度高温磁悬浮轴承试验台上使用所研制的高温位移传感器,能实现被悬浮物体的稳定悬浮。     

一种改进的航空发动机结构概率风险评估方法

针对航空发动机适航条款FAR33.75中关于发动机限寿件(ELLP)结构失效概率要求,提出了一种基于Kriging和蒙特卡罗半径外重要抽样(MCROIS)混合的结构概率风险评估方法。该方法针对ELLP高维、小失效概率事件以及极限状态函数为隐式、高度非线性的特点,利用Kriging元模型模拟隐式极限状态函数,然后通过主动学习迭代算法,计算最优点(MPP,最接近设计验算点的样本点),更新实验设计(DOE)并提高Kriging元模型的模拟精度。在此基础上,利用Kriging元模型确定最优抽样半径,构造半径外重要抽样密度函数,在最优抽样半径确定区域进行抽样,通过构造主动学习函数,使样本点更多落在抽样半径确定的球区域附近,加速失效概率计算的收敛,并构建了ELLP风险概率模型,解决了高维、小失效概率事件以及隐式、非线性极限状态函数的发动机结构概率风险评估难题,以某型发动机低压压气机轮盘为应用示例,与传统的蒙特卡罗仿真(MCS)方法进行了对比,验证了该方法的高效率、鲁棒性和仿真精度。     

武器舱气动噪声主动流动控制技术风洞试验研究

针对飞机弹舱高强度气动噪声、内埋武器分离安全性等问题,以高速风洞动静态压力测量技术为研究手段,开展了基于脉冲射流激励器（Powered Resonance Tubes,PRTB）的武器舱气动噪声抑制技术试验研究。试验结果表明,试验模型具有典型的开式空腔流动特点,武器舱内部非定常流动引起的声载荷可达到150dB。PIV 试验结果研究表明空腔前缘布置主动脉冲射流激励器对剪切层施加激励,会改变武器舱上部剪切层的流动特性,对这种高强度的声载荷起到一定的抑制作用。     

带执行装置的压气机系统建模及仿真

针对压气机主动稳定控制对模型的要求,以Moore-Greitzer模型为基础,首先将模型进行空间离散化,用平均分布在压气机周向环面的离散位置点来描述流量扰动,建立了反映压气机周向动态特性的多维状态空间模型;其次以喷气装置作为主动稳定控制系统的执行装置,通过分析加入喷气装置后对流动区域产生的质量和动量影响,同时考虑气流从喷气装置出口到压气机起始平面存在的时间滞后,建立了带执行装置的压气机系统动态模型.以某压气机为例,对压气机失速行为及喷气状态下对失速的抑制作用进行仿真,结果表明:所建立的模型可以反映压气机旋转失速动态过程,通过控制喷气流量能拓展压气机的稳定工作范围,有效抑制压气机失速,模型可用于压气机主动稳定控制系统分析与设计.