太阳风离子在月面的反射过程及对月面电场的影响

为探究月表磁异常区对太阳风离子产生反射的原理, 基于嫦娥二号卫星携带太阳风离子探测器的探测数据, 用单粒子模拟法反演太阳风离子运动, 并分析离子入射角和反射角的分布. 实验结果表明： 太阳风离子先被月壤向各方向大范围散射, 再被月面电场向天顶方向加速; 太阳风中, 月面有45~75 V电势, 该正电势对月面反射的太阳风离子有显著影响.     

Solar wind dynamic pressure and electric field as the main factors controlling Saturn's aurorae

The interaction of the solar wind with Earth's magnetosphere gives rise to the bright polar aurorae and to geomagnetic storms, but the relation between the solar wind and the dynamics of the outer planets' magnetospheres is poorly understood. Jupiter's magnetospheric dynamics and aurorae are dominated by processes internal to the jovian system, whereas Saturn's magnetosphere has generally been considered to have both internal and solar-wind-driven processes. This hypothesis, however, is tentative because of limited simultaneous solar wind and magnetospheric measurements. Here we report solar wind measurements, immediately upstream of Saturn, over a one-month period. When combined with simultaneous ultraviolet imaging we find that, unlike Jupiter, Saturn's aurorae respond strongly to solar wind conditions. But in contrast to Earth, the main controlling factor appears to be solar wind dynamic pressure and electric field, with the orientation of the interplanetary magnetic field playing a much more limited role. Saturn's magnetosphere is, therefore, strongly driven by the solar wind, but the solar wind conditions that drive it differ from those that drive the Earth's magnetosphere.     

地磁太阴日变化L的M2潮变化特征

用M2潮引起的地磁太阳日变化L的谐波分析方法,计算了佘山地磁台的磁偏角、水平和垂直分量L的谐波系数。分离出海洋和电离层发电机对L的贡献,讨论了太阳活动对地磁太阳日变化的影响,并把结果与国外部分台站的结果进行了对比分析。     

甚低频电磁波方法预报地磁暴

通过观察甚低频电磁波的相位变化,预测太阳耀斑的级别.当太阳耀斑爆发时,太阳表面首先会发出大量电磁辐射(主要是X射线),甚低频电磁波能很好地感应到此辐射;其次还喷射出大量带电低能粒子流,这会引起地磁暴,且通常在耀斑爆发1~2d之后到达地球.给出了一个预报地磁暴的实例.两事件的时间间隔约为28h,太阳风的速度约为1 484.1km/s.     

地磁场的起源问题

关于地磁场的起源,至今仍是一个没有得到解决的问题。相关的解释很多,如：永磁体假说,电荷旋转假说,热压电效应解释,温差电效应解释,自激发电机假说等,但由于都存在着一些自身无法解决的问题而未能被广泛接受。地球周围有一个被称为范爱伦带的带电粒子连续分布。是范爱伦带产生了地磁场,还是地磁场产生了范爱伦带？经过考察,可能是后者。但是,地磁场的起源问题仍然不能由此得到解决,仍是一个未解之谜。     

月球探测的进展与我国月球探测的科学目标

在简述月球探测的历程与趋势的基础上,强调当代月球探测的总体目标为：(1)研究月球与地月系的起源和演化,特别是月球大气层与磁场的消失,矿物与岩石的分布和形成环境、月壤和内部层圈结构的形成以及月球演化的历程;(2)探测月球的资源、能源和特殊环境的开发利用及对人类社会长期可持续发展的支撑。我国不载人月球探测划分为绕、落及回三个阶段。为了全球性、整体性重新认识月球,绕月卫星探测的科学目标为获取全月面三维影像,探测14种有用元素的全球分布与丰度,探测月壤厚度并估算^3He资源量以及太阳活动对空间环境的影响。“落”为月球探测器软着陆就位探测和月球车巡视探测,建立月基光学、低频射电和极紫外天文观测平台。“回”为月球探测器软着陆就位探测和取样返回地面。     

奥氏体不锈钢氮离子注入层的研究

本文用俄歇能谱仪（ＡＥＳ），结合高精度表面轮廓仪测定奥氏体不锈钢氮离子注入层深度及氮浓度分布．用超显微硬度计（试验载荷为０．１ｇ至２．０ｇ）测量注入层的本征硬度，还用ｘ射线低角度掠射技术（ＧＩＸＲＴ）分析注入层的组织结构．研究结果表明：氮离子注入层为过饱和氮的单相国溶体非晶态层，它强化了奥氏体不锈钢表层，提高耐磨性，降低摩擦系数．注入态的耐蚀性优于非注入态．     

阴阳历日期互换的计算

以回归年和朔望月为基础,推导出阴、阳历日期换算公式。其依据是以给定阴历为起点,经过若干整回归年,导出现在的阳历日期,本文共有3种公式。反之,再由阳历向阴历换算,又有3种公式。     

地磁太阴日变化L的O1分量的变化特征

 用Winch提出的地磁太阴日变化分析方法确定佘山地磁台的地磁太阴日变化的O₁分量L(O₁).首先把佘山台 196 0～1988年D,H和Z各分量的时均值资料做为整体分析年平均变化,然后按季节和太阳活动性细分后进行计算分析.讨论了L(O₁)的基本特征和季节变化、电离层和海洋发电机效应对L(O₁)的影响以及太阳活动对L(O₁)的贡献,并与国外一些地磁台的结果进行了对比分析.     

Global inventory of Helium-3 in lunar regoliths estimated by a multi-channel microwave radiometer on the Chang-E 1 lunar satellite

Helium-3 (³He) implanted by solar wind in the lunar regolith is a valuable resource because of its potential as a fusion fuel. On the basis of the Apollo regolith samples, a linear relationship between ³He abundance and solar wind flux, optical maturity and TiO₂ content has been presented. China successfully launched its first lunar exploration satellite Chang-E 1 (CE-1) on October 24, 2007. A multi-channeled microwave radiometer was aboard the satellite with the purpose of measuring microwave thermal emission from the lunar surface layer. From the multi-channel brightness temperature (T_b) observed by CE-1, the global distribution of the regolith thickness was inverted from the multi-channel T_b, and was used to evaluate the total amount of ³He per unit area in the lunar regolith. The global inventory of ³He was estimated as being 6.6×10⁸ kg; 3.7×10⁸ kg for the lunar nearside and 2.9×10⁸ kg for the lunar farside.     

月球表面光度行为的地域依赖性分析

月球表面光度行为描述了月表物质反射的太阳光随入射、出射和太阳相角的变化,它取决于月壤颗粒的粒径和形状、孔隙度、粗糙度等物理特性和矿物成分等化学性质．本文利用嫦娥一号干涉成像光谱仪（IIM）2A级辐亮度数据,基于太阳相角一辐亮度二维直方图统计,可将月球表面划分为两种光度行为迥异的地域类型,二者FeO含量分别与月海和高地的值大致吻合．高地（阿波罗16号着陆点）和月海（澄海）区域的IIM数据验证了该划分方法的合理性．本文提出的直接依据IIM2A级数据太阳相角一辐亮度二维直方图的划分方法,可以避免FeO含量划分月表光度单元中由于后期数据处理过程引入的误差．     

地磁导航中载体涡流干扰场特性的仿真分析

地磁导航中的测量误差是影响地磁导航精度的关键因素,而包括涡流磁场在内的载体干扰磁场是产生误差的主要因素。目前各种运载体大量使用铁磁性材料,这样不可避免地会引起涡流磁场等干扰磁场。因此文中采用COMSOL Multiphysics仿真软件,建立了高速运动载体的涡流干扰场仿真模型。首先研究了永磁体与匀强磁场之间的关系,发现永磁体的剩磁越强,匀强场也越强,为模拟地磁场提供了理论依据。其次分析了载体在匀速转动时涡流磁场对地磁测量的影响,最后研究了载体摆动时的涡流场的分布。结果表明涡流磁场随着速度的增大而增强,且涡流磁场主要分布于载体中间位置。仿真结果为下一步地磁导航中的误差建模以及磁场校正技术的研究提供了理论依据。     

地磁活动指数与太阳活动的小波分析

根据1957—2012年的地磁指数Ap、Dst、AE和太阳活动参数(太阳黑子相对数R与太阳射电流量F10.7)数据,利用小波分析方法研究了地磁活动与太阳活动的关系.结果表明,Ap、Dst、AE指数和太阳活动参数均存在准11 a和准22 a的周期特征.Ap和AE峰值滞后于太阳参数峰值1~2 a;而Dst指数与太阳参数存在近似负相关的关系,但从第21太阳周起逐渐延迟于太阳参数,表明地磁活动受太阳活动影响的滞后性.此外,地磁指数峰值从第20太阳周开始有逐渐下降的趋势,反映了地磁活动对太阳活动的响应减弱.     

Production of iron nanoparticles by laser irradiation in a simulation of lunar-like space weathering

'Space weathering' is the term applied to the darkening and reddening of planetary surface materials with time, along with the changes to the depths of absorption bands in their optical spectra. It has been invoked to explain the mismatched spectra of lunar rocks and regolith, and between those of asteroids and meteorites. The formation of nanophase iron particles on regolith grains as a result of micrometeorite impacts or irradiation by the solar wind has been proposed as the main cause of the change in the optical properties. But laboratory simulations have not revealed the presence of these particles, although nano-second-pulse laser irradiation did reproduce the optical changes. Here we report observations by transmission electron microscopy of olivine samples subjected to pulse laser irradiation. We find within the amorphous vapour-deposited rims of olivine grains nanophase iron particles similar to those observed in the rims of space-weathered lunar regolith grains. Reduction by hydrogen atoms implanted by the solar wind is therefore not necessary to form the particles. Moreover, the results support the idea that ordinary chondrites came from S-type asteroids, and thereby provides some constraints on the surface exposure ages of those asteroids.     

地磁要素年均值的太阳周期变化

本文利用我国部分标准地磁台的观测资料,分析研究了地磁通日、静日和静日午夜年均值与周期远小于一年的短期扰动关系。结果表明,磁暴和地磁周日变化等短期扰动不同程度地影响了通日年均值,地磁年均值的太阳周期变化(长期变化)中含有短周期扰动的贡献。     

An impact-driven dynamo for the early Moon

The origin of lunar magnetic anomalies remains unresolved after their discovery more than four decades ago. A commonly invoked hypothesis is that the Moon might once have possessed a thermally driven core dynamo, but this theory is problematical given the small size of the core and the required surface magnetic field strengths. An alternative hypothesis is that impact events might have amplified ambient fields near the antipodes of the largest basins, but many magnetic anomalies exist that are not associated with basin antipodes. Here we propose a new model for magnetic field generation, in which dynamo action comes from impact-induced changes in the Moon's rotation rate. Basin-forming impact events are energetic enough to have unlocked the Moon from synchronous rotation, and we demonstrate that the subsequent large-scale fluid flows in the core, excited by the tidal distortion of the core-mantle boundary, could have powered a lunar dynamo. Predicted surface magnetic field strengths are on the order of several microteslas, consistent with palaeomagnetic measurements, and the duration of these fields is sufficient to explain the central magnetic anomalies associated with several large impact basins.     

日月食限的计算

日月食的观测对太阳物理学、天文学及其它相关学科的研究有重要意义．然而准确的日月食预报却离不开日月食限的计算．本文研究了日月食计算方法，力求简单易懂，以便于课堂教学和进行科普教育．     

Planetary science: constant illumination at the lunar north pole

Images returned by the spacecraft Clementine have been used to produce a quantitative illumination map of the north pole of the Moon, revealing the percentage of time that points on the surface are illuminated during the lunar day. We have used this map to identify areas that are constantly illuminated during a lunar day in summer and which may therefore be in permanent sunlight. All are located on the northern rim of Peary crater, close to the north pole. Permanently sunlit areas represent prime locations for lunar outpost sites as they have abundant solar energy, are relatively benign thermally (when compared with equatorial regions), and are close to permanently shadowed regions that may contain water ice.     

A non-terrestrial 16O-rich isotopic composition for the protosolar nebula

The discovery in primitive components of meteorites of large oxygen isotopic variations that could not be attributed to mass-dependent fractionation effects has raised a fundamental question: what is the composition of the protosolar gas from which the host grains formed? This composition is probably preserved in the outer layers of the Sun, but the resolution of astronomical spectroscopic measurements is still too poor to be useful for comparison with planetary material. Here we report a precise determination of the oxygen isotopic composition of the solar wind from particles implanted in the outer hundreds of nanometres of metallic grains in the lunar regolith. These layers of the grains are enriched in 16O by >20 +/- 4 per thousand relative to the Earth, Mars and bulk meteorites, which implies the existence in the solar accretion disk of reactions--as yet unknown--that were able to change the 17O/16O and 18O/16O ratios in a way that was not dependent strictly on the mass of the isotope. Photochemical self-shielding of the CO gas irradiated by ultraviolet light may be one of these key processes, because it depends on the abundance of the isotopes, rather than their masses.     

基于最小二乘的地磁场测量误差补偿技术研究

地磁导航中获取地磁场的精确测量值是进行地磁匹配导航的前提和基础。论文针对实际地磁测量中磁力仪易受环境磁场干扰带来的影响补偿效果的问题，首先分析了软磁误差以及硬磁误差对磁场测量的影响效果，建立了地磁测量误差的参数化模型。采用ANSYS仿真软件，通过3对内径不同的亥姆霍兹线圈产生了3个方向的匀强磁场，从而实现了对地磁场的模拟。在此基础上，将磁力仪和干扰源建到仿真模型中，通过360度旋转磁力仪分别得到了有干扰和无干扰时的三维磁场值，然后采用最小二乘算法对模型参数进行了估计，最终实现了对磁场测量误差的补偿。仿真结果表明，该方法简单易行，简化了参数的求解过程，具有较高的误差补偿能力，地磁测量误差可以从20 000多纳特减少到几个纳特。