1998年5月日冕三维结构的数值模拟

采用三维理想磙流体力学（MHD）模式，内边界条件把二维投影特征线边界方法推广应用到三维计算，有效地稳定了数值计算并保证稳态解的自洽性；初始猜解磁场由1935卡林顿周光球磁场观测数据得到，这样计算得到的1998年5月份期间日冕三维结构比较符合实际，计算结果表明：（1）计算得到的源表面非径向磁场量值在磁中性线附近不超过2μT，表明源表面磁场基本径向。（2）模拟得到的源表面径向磁场量值除了在磁中性线附近的区域外变化不大，这和观测一致。（3）由源表面磁场按平方反比的规律计算出1AU处磁场量值更接近观测值。（4）计算得到的日冕结构和观测定性一致，三维数值模拟结果表明，日冕的三维大尺度背景结构主要是由磁场决定的，在闭磁场处或者电流片附近，太阳风的密度高，速度低；在开场区，太阳风的密度低，速度高。     

一个基于观测的太阳风背景模型

建立由太阳光球磁场和日冕偏振亮度等观测约束的单流体太阳风模型,包括日冕和太阳风的等离子体密度、速度和磁场,温度还有待于以后处理.这里采用高山观测台(HAO)MKⅢ的日冕偏振亮度(pB)在1.36Rs上的观测概图,根据Guhathakurta在1996年发展的日冕电子密度反演模型确定日冕的电子密度分布.同时采用Wilcox太阳观测台(WSO)的光球磁场视向分量的观测概图作为底部边界,根据Zhao等在1994年发展的水平电流-电流片(HCCS)模型得到全球磁场.Phillips在1995年及McComas在2003年分别用Ulysses第一次和第二次跨极飞行的观测发现,归一化到1 AU的太阳风动量流密度除了在10°～30°的纬度范围内略低以外几乎不变.根据这一结论,结合已经得到的密度数据,就可以得到日冕和太阳风的速度.将上面的模型应用于1918卡林顿自转周稳态太阳风的研究,结果与太阳活动极小期的观测基本相符,但是与观测相比较低速高密度区偏大,因此密度模型还有待改进.      

两冕流间CME事件数值模拟的改进

通过偶极子场和六极子场适当叠加，改进猜解磁场，使猜解磁场在太阳南北极符号相反，然后采用理想磁流体力学方程组(MHD)，由猜解磁场与太阳风流动相互作用计算出稳态自洽解，得到定性上与观测比较接近的具有两个冕流的背景结构．在两个冕流间采用具有同心圆磁场位形的触发模型触发CME事件，研究CME的日冕传播特征．模拟结果表明，CME被约束在两冕流间传播，CME闭磁场位形和磁云横截面磁场位形相似，可以解释1AU处观测磁云的部分特征；在CME附近，存在压力和Lorentz力起主要作用的区域，这可以为分析1AU处CME事件的观测数据提供帮助．     

WSA太阳风经验模型及其应用

Wang-Sheely-Arge （WSA）模型是对准稳态太阳风的经验和物理相结合的描述,其利用观测的日面磁图作为输入,可以提前3到4天预测L1点处的太阳风速度和行星际磁场极性.WSA模型是在WS模型的基础上经过若干改进形成的实时预报模式,之后又借鉴Distance from the Coronal Hole Boundary （DCHB）模型的参数,进一步改进了太阳风速度关系式,形成了目前常见的形式.WSA经验模型由日冕磁场模型、太阳风速度关系式和一维运动学模型三部分组成.在实际应用过程中,基本步骤包括观测磁图预处理、日冕三维磁场反演、计算日冕磁场参数、计算太阳风的速度分布和将太阳风映射到1AU等环节.在发展过程中,WSA模型经历了一些细节上的调整变化,例如观测磁图数据的来源、日冕磁场模型的类型、经验速度关系中自由系数的取值等.许多研究对如何改善模型的预报效果进行了探索.      

1991年太阳L260°活动概况及其射电的特征

本文介绍了太阳L260°活动概况,并计算了黑子群的位置漂移及对应的射电缓变源.北京天文台2.84GHz射电望远镜在该活动区观测到8次特大的射电爆发(流量超过1000s.f.u.),其中4次(1991年5月16日,6月9日,6月11日,8月25日)射电爆发时变曲线十分相似而且这些微波爆发都与Ⅱ型Ⅲ型Ⅳ型米波爆发有良好的对应.可能说明该活动区所对应的日冕在长时间内存在一种磁场位形结构,这种磁场位形结构容易产生日冕物质抛射.      

多种观测数据驱动的三维行星际太阳风MHD模拟

三维磁流体力学（MHD）数值模拟是行星际太阳风研究的重要手段.本文发展了一种由多种观测数据驱动的三维行星际太阳风MHD数值模型.模型的计算区域为0.1AU到1AU附近，使用Lax-Friedrich差分格式在六片网格系统中进行数值求解.边界条件中磁场使用GONG台站观测的光球磁图外推获得，密度通过LASCO观测的白光偏振亮度反演得到，速度根据以上两种观测数据并利用一种基于人工神经网络技术（ANN）的方法得到，温度通过自洽方法根据磁场和密度导出.利用该模型模拟了第2062卡灵顿周（CR2062）时期的行星际太阳风，模拟结果显示出丰富的观测特征，并与OMNI以及Ulysses的实际观测值符合得较好.该模型可用于提供接近真实的行星际太阳风，有助于提高空间天气预报的精度.      

基于CPU/GPU的日冕偏振亮度并行计算模型

三维磁流体力学(MHD)数值模拟是用来研究日冕和太阳风最常用的方法之一, 其中将计算得到的日冕电子数密度转化为日冕偏振亮度(Polarization Brightness, PB)是与观测对比的重要方法. 由于待转换电子数据网格密度、PB数据网格密度和计算模型的复杂度, 使得日冕偏振亮度的计算比较耗时, 利用单CPU计算无法达到近实时转换日冕偏振亮度的要求, 从而影响了数值模拟的验证效率. 本文在CPU/GPU环境下, 利用CUDA编程技术, 提出了一个日冕偏振亮度并行计算模型. 实验结果表明, 该模型比CPU上的串行模型计算速度提高了31.86倍, 达到了近实时模拟与观测数据比对的计算要求.      

日冕环和日冕拱的平衡位形

在线性场近似条件下,本文讨论了日冕环的二维平衡位形。用富利叶变换的方法,求出了问题的分析解,解释了日冕环观测结果的主要特性。沿日冕环纵向的压力分布均匀,日冕环的位形可以比无力场更稳定。由于日冕环可以储存更多的剪切场或扭转场的磁能,释放这部分磁能就可以驱动日冕环运动产生日冕瞬变过程,或者使环内的等离子体加热或加速而产生太阳耀斑。      

球坐标系六片网格下三维定态行星际太阳风模拟

采用二阶MacCormack差分格式, 利用稳态的磁流体(MHD)方程组在球坐标系六片网格下模拟研究了行星际太阳风. 六片网格系统能有效避免极区奇性和网格收敛性. 迭代按径向方向推进求解, 很大程度上减少了计算量, 节约了计算时间. 内边界条件根据太阳与行星际观测确定, 比较测试了5种内边界条件, 模拟给出了1922卡林顿周的背景太阳风结构. 几种内边界条件所得模拟结果与行星际观测基本吻合. 太阳风速度采用McGregor 等的经验公式给出, 磁场由水平电流片(HCCS)模型得到, 密度和温度分别根据动量守恒和气压守恒得到, 研究表明采用这样的边界条件模拟结果最佳.      

火星磁层顶形成和变化的理论研究

考虑太阳风动压与行星电离层中的带电粒子热压及磁压之和平衡,建立了有大气（电离层）的行星磁层顶形成的理论模型,结合卫星对火星的观测数据,对子午面内向日侧火星磁层顶位形进行了数值计算和分析,研究了火星磁层顶位形及其与太阳风动压之间的变化关系．结果认为,火星磁层顶位形与地球磁层顶相似．太阳风动压越大,火星磁层顶越靠近火星;太阳风动压越弱,火星磁层顶越远离火星．根据火星内秉磁矩从古到今逐渐减小的观点,探索了大尺度磁场（内禀磁矩）对火星磁层顶的贡献作用,结果认为大尺度磁场越强,火星磁层顶越远离行星．这对于进一步研究火星磁层的长期演化以及其他行星磁层的位形变化都具有重要的意义．     

Learning in an immersive digital theater

The Houston Museum of Natural Science, in collaboration with Rice University has an outreach program taking portable digital theaters to schools and community sites for over five years and has conducted research on student learning in this immersive environment. By using an external independent evaluator, the effectiveness of NASA-funded Education and Public Outreach (EPO) projects can be assessed. This paper documents interactive techniques and learning strategies in full-dome digital theaters. The presentation is divided into Evaluation Strategies and Results and Interactivity Strategies and Results. All learners from grades 3–12 showed statistically significant short-term increase in knowledge of basic Earth science concepts after a single 22-min show. Improvements were more significant on items that were taught using more than one modality of instruction: hearing, seeing, discussion, and immersion. Thus immersive theater can be an effective as well as engaging teaching method for Earth and Space science concepts, particularly those that are intrinsically three-dimensional and thus most effectively taught in an immersive environment. The portable system allows taking the educational experience to rural and tribal sites where the underserved students could not afford the time or expense to travel to museums.     

Stochastic particle acceleration by the forced interaction of relativistic current sheets

We address the problem of interacting relativistic current sheets in self-consistent kinetic plasma simulations within the framework of the Particle-In-Cell model. The interaction is enforced in head-on collisions of up to 10 current sheets at relativistic bulk speeds. The simulations are motivated by the general problem of Poynting flux dissipation in ‘striped wind’ configurations presumably governing the relativistic outflows pervasive in pulsar winds and gamma-ray bursts. We identify the generation of non-thermal particles and formation of a stable power-law shape in the particle energy distributions f(γ) dγ ∝ γ^−s dγ. In 1D, a spectral index s ∼ 2 is observed and attributed to a stochastic Fermi-type acceleration mechanism. In 2D, the generic index of s ∼ 3–4 is retained as in previous simulations of individual current sheets. Whereas in 2D the high energy cut-off is constrained by the limited dissipation of magnetic energy, in 1D the process converts the bulk motion of current sheets towards directed particle momentum of an exclusive class of non-thermal particles.     

Scaling analysis and model estimation of solar corona index

A monthly average solar green coronal index time series for the period from January 1939 to December 2008 collected from NOAA (The National Oceanic and Atmospheric Administration) has been analysed in this paper in perspective of scaling analysis and modelling. Smoothed and de-noising have been done using suitable mother wavelet as a pre-requisite. The Finite Variance Scaling Method (FVSM), Higuchi method, rescaled range (R/S) and a generalized method have been applied to calculate the scaling exponents and fractal dimensions of the time series. Autocorrelation function (ACF) is used to find autoregressive (AR) process and Partial autocorrelation function (PACF) has been used to get the order of AR model. Finally a best fit model has been proposed using Yule-Walker Method with supporting results of goodness of fit and wavelet spectrum. The results reveal an anti-persistent, Short Range Dependent (SRD), self-similar property with signatures of non-causality, non-stationarity and nonlinearity in the data series. The model shows the best fit to the data under observation.     

Development of a gas chromatography compatible Sample Processing System (SPS) for the in-situ analysis of refractory organic matter in martian soil: preliminary results

In the frame of the 2009 Mars Science Laboratory (MSL) mission a new sample preparation system (SPS) compatible with gas chromatography–mass spectrometry (GC–MS) has been developed for the in situ analysis of complex organic molecules in the Martian soil. The goal is to detect, if they exist, some of the key compounds that play an important role in life on Earth including carboxylic acids, amino acids and nucleobases.     

基于LuGre模型的电液加载系统摩擦补偿

为了提高电液加载系统控制精度,针对摩擦问题提出了基于LuGre摩擦模型的前馈补偿方法.建立了用于摩擦仿真分析和补偿器设计的电液加载系统数学模型;通过实验获取并分析了相关的摩擦数据;基于实验数据进行LuGre模型参数辨识,把LuGre模型和辨识结果引入电液加载系统数学模型,并进行仿真结果与实际摩擦数据的对照,证明了LuGre摩擦模型的准确性.设计前馈补偿器,进行了实验对比,实验结果表明前馈补偿器可将摩擦产生的控制误差有效地降至未补偿时的30%左右.      

CoRoT and Kepler results: Solar-like oscillators

The space-borne observatories CoRoT (Convection Rotation and planetary Transits) and Kepler have provided photometric time series data of unprecedented precision for large numbers of stars. These data have revolutionized the fields of transiting exoplanets and asteroseismology. In this review some important asteroseismic results obtained using data from the CoRoT and Kepler space missions concerning stars that show solar-like oscillations are discussed. These results comprise, among others, measurements of the location of the base of the convection zone and helium second-ionization zone in main-sequence stars, the presence (or not) of core-helium burning in red-giant stars, as well as differential rotation in these stars.     

Radioactivity of the Moon and planets

In this report the main results of the study of radioactivity of the solar sistem bodies are considered. The radioactivity of the Moon and planets was measured by means of vehicles in situ. The radioactivity of the lunar samples, brought to the Earth was studied with laboratory equipment.     

Return to Europa: Overview of the Jupiter Europa orbiter mission

Missions to explore Europa have been imagined ever since the Voyager mission first suggested that Europa was geologically very young. Subsequently, the Galileo spacecraft supplied fascinating new insights into this satellite of Jupiter. Now, an international team is proposing a return to the Jupiter system and Europa with the Europa Jupiter System Mission (EJSM). Currently, NASA and ESA are designing two orbiters that would explore the Jovian system and then each would settle into orbit around one of Jupiter’s icy satellites, Europa and Ganymede. In addition, the Japanese Aerospace eXploration Agency (JAXA) is considering a Jupiter magnetospheric orbiter and the Russian Space Agency is investigating a Europa lander.     

基于最小值原理的冗余度机器人动力学控制

为了解冗余度机器人全局法优化中数值求解的困难,本文讨论了动力学方程的建立,无约束和有约束最优控制问题之间的内在联系,重点分析了求解最优控制问题的数值方法,文中提出了双向异步积分迭代的求解正则方程组的直接迭代法,较好解决了状态方程和协态方程稳定相逆给求解两点这值问题带来的困难。     

基于GPS载波相位的微卫星姿态算法研究

GPS姿态系统是利用GPS载波相位测量来确定载体的航向和姿态角。本文对微卫星的GPS姿态系统进行了研究。重点解决短基线的GPS状态算法，讨论了姿态价格函数的了小化方法。测试结果表明，所提的算法对小于1m的基线是有效的。