The Genesis Solar Wind Concentrator Target: Mass Fractionation Characterised by Neon Isotopes

The concentrator on Genesis provided samples of increased fluences of solar wind ions for precise determination of the oxygen isotopic composition. The concentration process caused mass fractionation as a function of the radial target position. This fractionation was measured using Ne released by UV laser ablation and compared with modelled Ne data, obtained from ion-trajectory simulations. Measured data show that the concentrator performed as expected and indicate a radially symmetric concentration process. Measured concentration factors are up to ∼30 at the target centre. The total range of isotopic fractionation along the target radius is 3.8%/amu, with monotonically decreasing ²⁰Ne/²²Ne towards the centre, which differs from model predictions. We discuss potential reasons and propose future attempts to overcome these disagreements.     

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.     

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.     

煤基喷气燃料代用组分神经网络混合构建方法

为了建立航空燃料的喷雾模型,用于高保真液雾燃烧数值模拟,提出了基于人工神经网络混合模型的煤基喷气燃料代用组分构建方法.基于这一构建方法,重点针对煤基喷气燃料的雾化特性,利用多组分混合燃料的理化性质数据库对神经网络进行训练,获得了混合燃料理化性质隐式预测模型,结合随机投点优化方法,构建出能够很好地模拟煤基喷气燃料目标理化性质的代用组分.结果表明:该代用组分包含了5种碳氢化合物成分,摩尔分数为11.46%正癸烷、23.29%正十二烷、49.87%正十四烷、6.66%异辛烷和8.72%甲基环己烷.通过雾化特性实验,验证了代用组分对真实燃料雾化性能的模拟效果.该代用组分构建方法可以较好地解决混合燃料模拟过程中的非线性问题,通过改变目标理化性质可构建出相应代用组分.      

一级旋流强度对双旋流杯下游油气分布的影响

为了改善双旋流杯点火性能,需要优化其下游的流场和油雾场。利用激光粒子动态分析技术(PDA)测量基准双旋流杯下游的流场和油雾场,据此提出一级旋流器旋流数仅增大6.7%,但切向动量矩减小44%的改进方案,并进行了流场和油雾场对比试验。试验结果表明:减小双旋流杯一级旋流切向动量矩会使旋流杯下游流场结构发生较大变化,使其从收扩型转变为扩张型,同时减小油雾的索太尔平均直径(SMD);当与旋流杯出口距离超过2.5倍文氏管喉道直径时,流场输运和油滴蒸发作用增强,使得油雾分布更加均匀,燃油SMD更小。在航空发动机燃烧室双旋流杯设计中,不仅要考虑传统的旋流数概念,还应考虑各级切向动量矩的综合影响作用。     

弱旋流喷嘴的污染排放和燃烧稳定性分析

基于弱旋流喷嘴(LSI)的弱旋流燃烧技术具有极低的NOx污染排放能力.分析了弱旋流燃烧的稳定燃烧和降低污染排放的原理,发现其特殊的流动形式及其与湍流火焰传播的匹配是决定其燃烧稳定性和污染排放的主要因素.而弱旋流喷嘴的旋流叶片角度、直径比和流量比等关键参数会影响LSI的下游流动特征,进而影响其燃烧性能.燃料对LSI燃烧稳定性和污染排放的影响主要是通过火焰传播速度和绝热火焰温度发挥作用.为了将液体燃料应用于LSI,目前主要采用了预混预蒸发的方式,试验结果表明:其NOx排放可比采用常规强旋流喷嘴的燃烧室降低10%~60%,但存在自燃和回火的风险.而LSI喷雾燃烧的方式,则需要针对弱旋流液雾燃烧开展更深入的基础研究.只有解决了液体燃料的LSI应用问题,才能发展出不同于传统强旋流燃烧的新一代航空发动机超低排放燃烧室.      

以柴油为燃料的燃烧室燃烧效率实验及分析

地面动力常常需要改进利用航空燃气轮机技术,为了研究燃气轮机燃烧室在低工况下使用柴油燃料的燃烧效率问题,采用燃气分析试验方法,对燃气轮机燃烧室在不同进口总温、空气流量和油气比等工况下的燃烧效率进行了研究。结果表明:油气比较低时,燃烧区温度低,燃烧不完全导致燃烧效率急剧下降,随着燃烧室油气比的增加,燃烧效率逐渐接近100%;进口空气流量以及进口总温的增加会提高空气雾化喷嘴的雾化能力以及燃烧温度,燃烧更加充分完全,燃烧效率由96%左右提高至99%以上;总结归纳得到了适用于柴油燃料的燃烧效率预估经验关系式。     

Boundary discontinuous Fourier analysis of thick beams with clamped and simply supported edges via CUF

This paper presents an analytical solution for static analysis of thick rectangular beams with different boundary conditions.Carrera's Unified Formulation (CUF) is used in order to consider shear deformation theories of arbitrary order.The novelty of the present work is that a boundary discontinuous Fourier approach is used to consider clamped boundary conditions in the analytical solution,unlike Navier-type solutions which are restricted to simply supported beams.Governing equations are obtained by employing the principle of virtual work.The numerical accuracy of results is ascertained by studying the convergence of the solution and comparing the results to those of a 3D finite element solution.Beams subjected to bending due to a uniform pressure load and subjected to torsion due to opposite linear forces are considered.Overall,accurate results close to those of 3D finite element solutions are obtained,which can be used to validate finite element results or other approximate methods.