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.     

T-1A型高精度绝对重力仪

高精度绝对重力仪用于测量地球表面的重力加速度（g,常用值9.81 m/s2）,在精密计量、大地测量、地球物理、资源勘探等领域具有广泛应用。近年来,清华大学自主研制完成T-1与T-1A型高精度绝对重力仪,采用新型的自由落体装置、激光干涉测量技术和信号处理方法,可实现微伽量级不确定度的精密重力测量。本文主要介绍T-1A型高精度绝对重力仪的系统技术和测试结果,经过进一步工程化改进,该仪器有望实际应用于重力计量、地震研究等领域。     

油膜干涉测量翼型壁面摩阻低速风洞试验技术

油膜干涉试验可以定量测量得到模型壁面的摩擦应力,是开展摩阻特性研究的有力工具。通过对油膜干涉试验技术中的试验原理、试验方法、误差修正、数据结果分析等关键问题的研究,初步建立了试验系统,具备了开展模型壁面摩阻特性研究的试验能力。综合分析表面热膜试验结果与数值计算结果,在以模型弦长为特征长度,试验雷诺数 Re ＝1．3×106的条件下,翼型表面摩擦应力沿模型弦向的分布规律具有较好的一致性。     

基于蒙特卡罗方法的冷原子干涉仪物理仿真

由于现有的噪声分析方法无法很好地评估在复杂环境下冷原子干涉仪的输出特性,本文提出了一种新的冷原子干涉仪仿真方法,可以模拟大动态条件下各项噪声及其之间的耦合对冷原子干涉仪的影响。利用单粒子波包演化的处理方式对冷原子干涉仪进行全过程物理建模,并采取蒙特卡罗方法对大量确定初态的原子进行全过程统计,最终得到冷原子干涉仪在多种噪声同时存在的情况下的响应。该方法主要优势体现在能够对噪声耦合情形进行高精度仿真,并且可以根据实际数据对干涉仪输出进行实时处理,以提升冷原子干涉仪的性能指标。     

某航机燃烧室煤油改柴油燃烧特性研究

为了给某型航空发动机改为地面用柴油型燃气轮机的设计提供重要的技术支持,本文借助数值计算的方法,采用FLUENT稳态压力求解器、P1辐射模型和涡耗散破碎(EDU)燃烧模型对某航空发动机燃烧室在巡航工况和最大工况下煤油与柴油两种燃料的燃烧特性进行了计算及对比研究。得到了该燃烧室使用航空煤油(RP-3)和0号柴油的热态流场、空气流量分配、温度场、出口温度分布、污染物排放及头部燃油蒸发量。研究结果表明：当该燃烧室的燃料由航空煤油改为0号柴油后,燃烧室的热态温度场分布基本一致,流量分配最大差异在0.45%之内;燃烧效率降低约4.3%和NO、Soot排放量相当;出口温度分布和总压损失差异分别在1%和4.1%之内。     

Design and analysis of a truss deployable antenna mechanism based on a 3UU-3URU unit

Space deployable structures with large calibers, high accuracy, and large folding ratios are indispensable equipment in the aerospace field. Given that the single-DOF 3RR-3RRR deployable unit cannot be fully folded, this study proposes a 3UU-3URU deployable unit with two kinds of DOF: folding movement and orientation adjustment. First, based on the G-K formula, the DOF of the 3UU-3URU unit is analyzed. Then, the 3UU-3URU unit is used to construct a deployable truss antenna with a curved surface, and the DOF of the whole deployable antenna containing multiple 3UU-3URU units is calculated. The structural design of a deployable antenna with two loops is carried out with specific parameters and geometric relations. Next, a DOF simulation of a basic combination unit composed of three 3UU-3URU units is performed. Finally, a prototype of the basic combination unit is manufactured, and the DOF of the mechanism is experimentally verified.     

深空探测器无线电干涉测量开源数据处理系统构建及试验

为更好地开展深空无线电干涉测量试验,基于DiFX(Distributed FX,分布式FX型相关处理)、SPICE(Spacecraft Planet Instrument Camera-matrix Events,航天器行星仪器照相机矩阵事件)、HOPS(Haystack Observatory Postprocessing System,Haystack克天文台后处理系统)及AIPS(Astronomical Image Processing System,天文图像处理系统)等开源软件,搭建了一套可用于深空探测器信号相关处理的无线电干涉测量数据处理系统。首先介绍了该系统的整体架构及组成,然后介绍了系统各组成模块的功能及工作原理,最后利用该系统对嫦娥三号着陆器开展了观测试验,并对观测数据进行了处理。试验结果表明,该系统能成功实现深空航天器信号的相关处理、条纹拟合,以及时延解算等功能,有望为我国嫦娥五号任务及火星探测任务数据处理提供支持。     

基于装配过程的关键特性识别与控制方法研究

基于关键特性的质量控制技术是一种先进的质量控制方法,该方法通过对下层关键特性进行监控,间接地保证产品的质量.在装配误差积累传递分析的基础上,研究了装配关键特性定性分析和定量识别方法,再结合统计过程控制理论,开发了关键特性识别与控制系统软件.该软件在某型号飞机应急门装配应用中,能够准确快速地识别关键特性,并有效地进行控制分析.