太空行走100问（十四）

太空行走风险（上）80．航天员在太空行走中可能会遇到哪些风险？（1）太空环境因素方面的风险：①宇宙辐射 在近地空间的宇宙辐射属于电离辐射,主要有三个来源：地球辐射带、银河宇宙线和太阳粒子事件。     

月球表面次级中子辐射环境仿真研究

由于缺少磁场和大气,宇宙线高能粒子轰击月壤可以形成月球特有的强中子辐射环境,并对航天员和电子设备造成潜在威胁。文章采用蒙特卡罗方法仿真研究宇宙线高能粒子辐射与月壤成分核反应产生的次级中子能谱特征,给出不同太阳活动、不同月壤深度下月球中子能谱特征和空间分布特征。仿真结果表明,宇宙线高能粒子导致的次级中子随着月壤深度的增加先增大后减小,大约在1 m深度达到最大值,深度越深银河宇宙线诱发的中子贡献越大。相关结果可为我国后续载人月球探测任务的辐射防护设计提供参考。     

知识资料窗

知识资料窗探空火箭在近地空间进行探测和科学试验的火箭称为探空火箭。利用探空火箭可以在高度方向探测大气各层结构、成分和参数，研究电离层、地磁场、宇宙线、太阳紫外线和Ｘ射线、陨尘等多种日一地磁场现象。探空火箭比探空气球飞得高、比低轨道运行的人造地球卫星飞...     

共面圆轨道最省燃料小推力多次变轨研究

本文研究两个共面圆轨道之间最节省燃料的多次变轨过程。通过分析，得到滑行段起点和终点之间的解析关系式，解决了变轨次数增加带来的计算问题。给出了从近地圆轨道到同面同步轨道的最优多次变轨的计算结果，并进行了分析和讨论     

动能撞击偏转近地小天体研究进展

以近地小天体防御为背景,介绍了近地小天体的基本概念和物理特性,分析了超高速动能撞击偏转近地小天体的研究进展。讨论了超高速动能撞击近地小天体表面成坑形貌、相似律以及成坑过程中抛射物产生机制、演化过程和抛射物质量速度分布相似律。总结了基于结合点源假设、实验和数值模拟结果建立的超高速动能撞击小天体动量传递理论模型和相似律。分析了近地小天体的物理特性和撞击条件对动量传递系数的影响规律。归纳了超高速动能撞击偏转近地小天体研究中存在的问题,对超高速动能撞击防御小天体的发展趋势提出了若干建议。     

太阳敏感器/陀螺定姿算法研究

针对近地航天器故障模式或深空探测模式,研究了仅利用太阳敏感器和陀螺进行航天器定姿的方法.给出了姿态确定滤波模型,分析了影响定姿精度的主要因素,讨论了轨道日照角对定姿精度的影响.研究结果表明:该组合可实现航天器故障模式或深空探测模式中的低精度姿态确定;轨道日照角对定姿精度影响较大,有效的轨道日照角是确保太阳敏感器/陀螺姿态确定方法可行的关键.     

地球观测卫星小推力轨道控制方案仿真

本文讨论了近地太阳同步卫星小推力轨道控制仿真的特点、要求和问题.选用EARLY DESIRE高级语言在PDP-11小型计算机上成功地对卫星轨道控制方案进行了实时仿真,预测了目标轨道.它将在卫星系统实时仿真和卫星运行管理中发挥作用.     

载人近地小行星探测器系统质量减小途径探讨

为减小载人近地小行星探测器的系统质量,提出采用先期运送部分推进舱至小行星、可伸缩式舱体、发展核推进技术的3种技术途径。介绍了国内已有的载人近地小行星探测器的系统组成及其质量估算方法。在此基础上,结合一个载人登陆探测近地小行星的算例,给出了采用上述3种减小质量途径的载人探测器系统质量估算结果。对3种技术途径的探测器总质量减小效果进行了对比,对各技术途径的特点和难点进行了讨论。结果表明:3种技术途径均可有效地减小载人探测器系统的总质量,有助于提高载人近地小行星探测任务的可行性。     

卫星舱内宇宙辐射剂量测量分析

本文介绍了在我国返回式卫星舱内辐射剂量测量的一些结果，分析了轨道高度和舱体质量厚度对舱内剂量的影响。卫星舱内的复杂屏蔽引起各位置上的剂量有所不同，测量结果表明：最高和最低剂量点剂量水平之比在５００ｋｍ高度的轨道时为１．５８，在３００ｋｍ高度的轨道时为１．２３。本文还对近地空间的辐射危害及其防护问题进行了讨论。     

一种提高导航卫星星座自主定轨精度的方法研究

针对近地导航卫星仅利用星间测距进行自主定轨时,因无法消除星座整体旋转误差而导致长期自主定轨精度不高的问题,提出了利用拉格朗日导航卫星星座与近地导航卫星星座联合仅利用星间测距进行自主定轨的方法。建立了拉格朗日轨道导航卫星星座和近地导航卫星星座联合仅利用星间测距进行自主定轨的动力学模型和观测模型。利用扩展Kalman滤波（EKF）算法和星间测距信息实现了拉格朗日轨道导航星座与近地导航星座的长期自主定轨。以4颗拉格朗日卫星组成的导航星座与12颗GPS卫星组成的近地导航星座作为仿真对象进行了仿真分析,仿真结果表明本文仅利用星间测距的联合自主定轨方法可以有效提高导航卫星星座的长期自主定轨精度。
     

Cosmic ray impact on extrasolar earth-like planets in close-in habitable zones

Because of their different origins, cosmic rays can be subdivided into galactic cosmic rays and solar/stellar cosmic rays. The flux of cosmic rays to planetary surfaces is mainly determined by two planetary parameters: the atmospheric density and the strength of the internal magnetic moment. If a planet exhibits an extended magnetosphere, its surface will be protected from high-energy cosmic ray particles. We show that close-in extrasolar planets in the habitable zone of M stars are synchronously rotating with their host star because of the tidal interaction. For gravitationally locked planets the rotation period is equal to the orbital period, which is much longer than the rotation period expected for planets not subject to tidal locking. This results in a relatively small magnetic moment. We found that an Earth-like extrasolar planet, tidally locked in an orbit of 0.2 AU around an M star of 0.5 solar masses, has a rotation rate of 2% of that of the Earth. This results in a magnetic moment of less than 15% of the Earth's current magnetic moment. Therefore, close-in extrasolar planets seem not to be protected by extended Earth-like magnetospheres, and cosmic rays can reach almost the whole surface area of the upper atmosphere. Primary cosmic ray particles that interact with the atmosphere generate secondary energetic particles, a so-called cosmic ray shower. Some of the secondary particles can reach the surface of terrestrial planets when the surface pressure of the atmosphere is on the order of 1 bar or less. We propose that, depending on atmospheric pressure, biological systems on the surface of Earth-like extrasolar planets at close-in orbital distances can be strongly influenced by secondary cosmic rays.     

Energy measurements of electrons and protons in cosmic ray physics using satellite and balloon calorimeters in recent two decades

Calorimeters are used in cosmic ray studies for a variety of purposes, such as measurements of particle energy, separation of electrons and hadrons, formation of triggers (signals for activation of instruments), and so on. In this review we consider the methods of energy reconstruct of protons and electrons (for particles with energies exceeding 10 GeV) in calorimeters of various types that are used in astrophysical experiments of cosmic ray studies carried out with balloons and satellites.     

波纹板夹层结构高温钎焊焊缝X射线影像分析

为检测波纹板夹层结构高温钎焊焊缝质量,对其进行了X射线照相检查。波纹板夹层钎焊缝与一般熔焊焊缝不同,无论焊缝本身以及焊缝缺陷都有其特有的特点。本文通过对钎焊焊缝结构特点及焊缝X射线影像的分析,总结了获得高清晰X射线照片的方法及焊缝缺陷的识别特征。     

影响GEO卫星长寿命高可靠的空间环境因素及其评估、验证和保障技术研究

文章叙述了空间环境与卫星长寿命高可靠的关系,着重分析了影响GEO卫星长寿命高可靠的各种空间环境效应,如:地磁亚暴电子造成的卫星表面带电及诱导的二次放电、辐射带高能电子引起卫星内带电、太阳耀斑质子和银河宇宙射线造成的单粒子效应、空间带电粒子和太阳电磁辐照造成的辐照总剂量效应以及空间环境下敏感表面的污染效应等.文章最后给出GEO卫星空间环境效应的评估、验证和保障技术研究的必要性及其主要研究方向.     

Detection of ultrahigh-energy cosmic rays and neutrinos by radio method using artificial lunar satellites

An estimate of the feasibility of the ultrahigh-energy cosmic ray and neutrino detection using a lunar satellite-borne radio receiver is presented. The data obtained in the proposed experiment will make resolving the current contradictions in the ultrahigh-energy cosmic ray spectra measured with the major ground-based instruments possible. Moreover, they will enable us to considerably extend the accessible energy range and to check predictions of various models of the origin of the highest-energy particles in the Universe. At the same time the lunar radio detector provides a means of searching for ultrahigh-energy neutrinos with a high sensitivity combined with a very large target effective mass.     

基于射线追踪的快速雷达图像仿真方法

为了解决目标识别、隐身目标设计等研究领域对雷达图像需求日益增加的问题,提出了一种基于射线追踪的快速雷达图像仿真方法。该方法利用射线追踪计算每一个射线管的散射电场及其在雷达成像平面的投影坐标,通过将所有射线管的贡献在像域进行累加得到1幅二维雷达图像。通过对不同路径射线的聚类,可实现对散射贡献的分离,从而建立目标部件与强散射源的对应关系,并对复杂目标雷达图像进行解释。给出了Slicy目标的快速雷达图像仿真与算例分析,分析结果表明:基于射线追踪的快速雷达图像仿真方法可对复杂雷达图像进行有效预测,并能对强散射源进行成因分析。     

Short-term variation of cosmic ray diurnal anisotropy and solar activity

A correlative analysis has been made between cosmic ray intensity and solar activity (sunspot numbers) during high amplitude days for the period 1991–1995. The high amplitude days with the time of maximum in the corotational/azimuthal direction do not indicate any significant correlation with solar activity. The diurnal amplitude significantly remains constant and high (0.5%) during the entire period. Our observations suggest that the direction of the anisotropy of high amplitude anisotropic wave train events contribute significantly to the short-term behavior of the cosmic ray diurnal anisotropy. The correlation coefficient is found to remain positive during solar activity maximum for all the high amplitude anisotropic wave train events.     

Motion and transport of solar cosmic rays in heliospheric traps: The event on January 28–31, 2001

The results of studying the enhancement of solar cosmic ray fluxes on January 28?C31, 2001 in a wide energy range are presented using the ACE spacecraft data. A comparative analysis of temporal variations of the fluxes of charged particles and of the interplanetary medium parameters (interplanetary magnetic field and solar wind) has been performed on the basis of the ??reflection?? model of motion, accumulation, and modulation of cosmic rays. It is shown that a magnetic trap for solar cosmic rays was created by a plasma stream and flare ejection from an active region in the western part of the solar disk. Particles of low energies (<10 MeV) were captured inside the trap; the dispersion of distribution of particles with different energies inside the trap being determined by its complicated magnetic structure. The power-low dependence of the time of maximum for the flux of particles on their energy is found, and softer energy spectrum inside the trap is explained.