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.     

燃气涡轮无气膜冷却动叶参数化设计系统应用

为进行燃气涡轮冷却结构的设计,在考虑总的温度分布系数(OTDF)及不考虑OTDF两种情况下,采用一套设计方法,完成了燃气涡轮第一级动叶冷却结构的整体设计。通过设计表明:采用管网计算,并通过三维导热计算进行热分析,最后通过气热耦合计算能够快速地设计出较佳的冷却结构;不考虑OTDF设计时,第一腔流量为16.9g/s,第二腔流量为40.8g/s,最大无量纲温度0.700,采用双进口蛇形通道,换热效果较佳,且结构设计较为简单;考虑OTDF时,为达到设计要求,第一腔流量为18.2g/s,第二腔流量为25.4g/s,第三腔流量为5.3g/s,最大无量纲温度0.752。通过多方案设计,得出在无气膜情况下,采用三个冷气进口多回转通道能够达到较好的冷却效果。     

前缘参数对翼型气动-隐身特性敏感性分析

针对翼面部件对隐身飞机气动和隐身性能影响更为突出的问题,提出了一种翼型前缘参数化修形方法,采用高精度气动和电磁数值计算方法,进行了前缘形状对翼型气动-隐身特性的敏感性分析。研究结果表明:翼型前缘半径增加,其最大升力系数、失速迎角、最大升阻比显著增加,但其前向RCS均值也增加明显,设计时需进行综合权衡;在不影响结构和装载的情况下,下表面偏角尽量小,修形长度取0.15c,对翼型的低、高速气动和隐身特性都有利。     

高超声速飞行器机体/推进一体化设计的启示

机体/推进一体化设计是吸气式高超声速飞行器的关键技术。飞行器的前体和后体既是主要的气动型面,又是发动机进气道的外压缩型面和尾喷管的膨胀型面,一体化设计直接影响飞行器的气动与发动机性能。本文阐述了吸气式高超声速飞行器的主要特点,梳理了飞行器的推阻匹配、升阻比特性、操稳匹配等主要气动设计问题。通过对国外典型高超声速飞行器机体/推进一体化设计技术的综合分析,总结了前体/进气道、后体/尾喷管、边界层强制转捩装置等关键部件的气动设计方法,获得了有意义的启示,可为后续吸气式高超声速技术研究提供重要参考。     

高超声速气动热预测技术及发展趋势

高超声速气动热预测技术是高超声速飞行器发展的关键技术之一。对高超声速气动热预测技术的发展情况进行了分析探讨。首先,简要回顾了国内外高超声速气动热理论预测及地面实验技术的发展历程;在此基础上,结合典型外形的计算与风洞试验结果的比较,重点介绍分析了气动热工程计算方法、数值模拟方法、气动热风洞试验设备的模拟能力及目前实验测试技术的研究水平;最后,对气动热预测技术的发展趋势进行了讨论,提出了气动热预测技术应研究解决的问题。     

航天器贮箱变质量流固耦合系统的动力学响应

研究了航天器贮箱变质量流固耦合系统的动力学特性.根据虚拟质量法(VMM),结合边界元法和有限元法构建了系统的动力学模型,建模过程中着重考虑了质量变化对系统的动态影响.通过Newmark直接积分法计算出贮箱变质量系统的振动响应.结果表明:由于系统质量减少,引起了系统振动频率的增大,并产生一个附加负阻尼.系统的振动频率的范围可以通过系统质量的范围确定.变质量引起的附加负阻尼的大小与系统的质量变化率成正比.对于系统的横向振动,质量减少引起的附加负阻尼在整个过程对系统振动的影响比较稳定,对于系统的纵向振动,质量减少引起的附加负阻尼对系统振动的影响随时间的增加而增大.      

内冷通道横流条件下气膜冷却特性

为了研究内冷通道横流条件下气膜冷却的流动和换热特性,采用窄带瞬态液晶测量技术获得了内冷通道横流条件下吹风比分别为0.5,1,2时气膜孔下游冷却效率和表面传热系数云图,并通过数值模拟得到了气膜孔内及下游区域流场的详细信息.结果表明:内冷通道横流对气膜孔下游冷却效率和表面传热系数分布有重要的影响.横流增强了气膜孔射流的展向分布能力,增强了高吹风比时气膜冷却效果.另外,气膜孔下游涡的分布出现明显的不对称性,涡的结构更加复杂.      

变循环发动机组合变几何调节方案

基于面向对象的设计思想,设计出了一个双涵道变循环发动机(VCE)的性能计算模型,并选取了双涵道VCE具有代表性的典型工作点,进行了双涵道VCE的组合变几何调节的相关研究.结果表明:在双涵道VCE的亚声速巡航和超声速巡航工作点,合理调节风扇导流叶片角度可以更大程度发挥双涵道VCE性能优势;在亚声速巡航工作点时选取的方案4和超声速巡航工作点时选取的方案4均比双涵道VCE设计点的变几何调节方案性能更优.     

截锥不同冷却结构对喷管腔体红外抑制特征影响的数值研究

对发动机喷管高温部件之一的截锥3~5μm波段上红外抑制特征进行了数值研究.在红外辐射信号较强的截锥前端布置气膜缝槽冷却结构和气膜孔冷却结构,将温度较低的外涵气流通过支板引入截锥,有效降低了截锥、支板的壁面温度和红外辐射强度.对两种冷却结构进行比较,结果表明,采用向下气膜缝槽冷却结构能够达到较好的红外抑制效果,但推力损失较大;采用气膜孔冷却结构,喷管红外抑制效果略有减弱,但推力损失较小.