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.      

基于速度预测的导引律剩余时间估计

将分段线性逼近与迭代求解的思想扩展到对导弹的时变速度进行分段预测,给出了适用于反舰导弹速度时变情况的大前置角下比例导引律和偏置比例导引律的剩余时间估计算法。该算法在现有分段迭代算法的基础上,依据闭环形式的反舰导弹速度微分方程,分转弯平飞段和近似直线飞行段2种情况,对导弹未来速度的大小进行分段迭代预测并对剩余时间估计进行修正。算法中还给出了偏置比例导引律作用下近似直线飞行段剩余飞行航程的估计公式。仿真结果验证了本文算法的有效性。     

轨道参数对阿尔法磁谱仪太阳辐射热流的影响

为探明阿尔法磁谱仪（AMS）的温度变化规律,并为制定AMS的热控制方案提供指导和依据,推导了AMS重要区域（AMS前方、后方、顶部和左舷）的太阳辐射热流计算公式,分析了这些区域太阳辐射热流随轨道参数的变化,解释了AMS顶部的温度变化和太阳辐射热流变化规律在热控方案中的应用。分析表明在国际空间站（ISS）正常飞行姿态下,AMS前、后方和左舷的太阳辐射热流受太阳光与ISS轨道面的夹角（β角）、ISS与会日点的角距（θ角）和地球阴影区的影响,AMS顶部太阳辐射热流受β角和θ角的影响。得出结论：β角、θ角和地球阴影区均是影响AMS温度的主要因素,各区域的太阳辐射热流变化规律可以作为设计AMS温度控制方案的主要依据之一。     

基于光学测角数据的风云四号同步轨道卫星精密定轨

针对风云四号同步卫星的精密定轨和精度评估需求,首先利用地面光学测角数据对FY-4A卫星进行精密定轨,定轨后方位角和高度角的残差rms分别为0.25＂和0.45＂。与基于测距数据的轨道相比,位置精度在有测角数据的弧段内小于50m。进一步联合测角数据和测距数据对FY-4A卫星进行联合定轨,定轨后轨道重叠精度优于15m。利用联合定轨结果评估了基于测距数据的实时轨道产品精度,可以明显发现轨道精度随着测距数据的积累而逐步提高。     

Magnetic Field Fluctuations in the Solar Wind, Foreshock and Magnetosheath： Cluster Data Analysis

46 magnetosheath crossing events from the two years (2001.2-2003.1) of Cluster magnetic field measurements are identified and used to investigate the characters of the magnetic field fluctuations in the regions of undisturbed solar wind, foreshock, magnetosheath. The preliminary results indicate the properties of the plasma turbulence in the magnetosheath are strongly controlled by IMF orientation with respect to the bow shock normal. The amplitude of the magnetic field magnitude and direction variations behind quasi-parallel bow shock are larger than those behind quasi-perpendicular bow shock. Almost purely compressional waves are found in quasi-perpendicular magnetosheath.     

Structure of the Program of Short-term Prediction of Powerful Solar Flares

Input data of the system are two-dimensional images and one-dimensional distributions of total and polarized solar emission at 5.2 cm wavelength obtained with SSRT. Together with photoheliograms, magnetograms, Hα-filtergrams and characteristics of active regions received from other sources, they form the initial database. The first stage includes superimposing the images, identifying microwave sources with active regions, assigning NOAA numbers to the sources, and determining for each active region the heliolatitude, extent, and inclination angle of the group's axis to the equator. These data are used to calculate the boundaries of longitude zones for each active region. A next stage involves determining the brightness temperatures of microwave sources less than the polarization distribution, the degree of polarization, and microwave emission flux, as well as calculating the parameters of microwave sources. Each parameter is assigned its own value of the weight factor, and the sum of values is used to draw the conclusion about the flare occurrence probability in each active region and on the Sun in general.      

An adaptive fast fixed-time guidance law with an impact angle constraint for intercepting maneuvering targets

Sliding mode guidance laws based on a conventional terminal sliding mode guarantees only finite-time convergence, which verifies that the settling time is required to be estimated by selecting appropriate initial launched conditions. However, rapid convergence to a desired impact angle within a uniform bounded finite time is important in most practical guidance applications. A uniformly finite-time/fixed-time convergent guidance law means that the convergence (settling) time is predefined independently on initial conditions, that is, a closed-loop convergence time can be estimated a priori by guidance parameters. In this paper, a novel adaptive fast fixed-time sliding mode guidance law to intercept maneuver targets at a desired impact angle from any initial heading angle, with no problems of singularity and chattering, is designed. The proposed guidance law achieves system stabilization within bounded settling time independent on initial conditions and achieves more rapid convergence than those of fixed-time stable control methods by accelerating the convergence rate when the system is close to the origin. The achieved acceleration-magnitude constraints are rigorously enforced, and the chattering-free property is guaranteed by adaptive switching gains. Extensive numerical simulations are presented to validate the efficiency and superiority of the proposed guidance law for different initial engagement geometries and impact angles.     

Fundamental (f) oscillations in a magnetically coupled solar interior-atmosphere system – An analytical approach

Solar fundamental (f) acoustic mode oscillations are investigated analytically in a magnetohydrodynamic (MHD) model. The model consists of three layers in planar geometry, representing the solar interior, the magnetic atmosphere, and a transitional layer sandwiched between them. Since we focus on the fundamental mode here, we assume the plasma is incompressible. A horizontal, canopy-like, magnetic field is introduced to the atmosphere, in which degenerated slow MHD waves can exist. The global (f-mode) oscillations can couple to local atmospheric Alfvén waves, resulting, e.g., in a frequency shift of the oscillations. The dispersion relation of the global oscillation mode is derived, and is solved analytically for the thin-transitional layer approximation and for the weak-field approximation. Analytical formulae are also provided for the frequency shifts due to the presence of a thin transitional layer and a weak atmospheric magnetic field. The analytical results generally indicate that, compared to the fundamental value ($\omega =\sqrt{\mathit{gk}}$), the mode frequency is reduced by the presence of an atmosphere by a few per cent. A thin transitional layer reduces the eigen-frequencies further by about an additional hundred microhertz. Finally, a weak atmospheric magnetic field can slightly, by a few percent, increase the frequency of the eigen-mode. Stronger magnetic fields, however, can increase the f-mode frequency by even up to ten per cent, which cannot be seen in observed data. The presence of a magnetic atmosphere in the three-layer model also introduces non-permitted propagation windows in the frequency spectrum; here, f-mode oscillations cannot exist with certain values of the harmonic degree. The eigen-frequencies can be sensitive to the background physical parameters, such as an atmospheric density scale-height or the rate of the plasma density drop at the photosphere. Such information, if ever observed with high-resolution instrumentation and inverted, could help to gain further insight into solar magnetic structures by means of solar magneto-seismology, and could provide further insight into the role of magnetism in solar oscillations.     

Observation of a 27-day solar signature in noctilucent cloud altitude

Previous studies have identified solar 27-day signatures in several parameters in the Mesosphere/Lower thermosphere region, including temperature and Noctilucent cloud (NLC) occurrence frequency. In this study we report on a solar 27-day signature in NLC altitude with peak-to-peak variations of about 400?m. We use SCIAMACHY limb-scatter observations from 2002 to 2012 to detect NLCs. The superposed epoch analysis method is applied to extract solar 27-day signatures. A 27-day signature in NLC altitude can be identified in both hemispheres in the SCIAMACHY dataset, but the signature is more pronounced in the northern hemisphere. The solar signature in NLC altitude is found to be in phase with solar activity and temperature for latitudes $?70°$N. We provide a qualitative explanation for the positive correlation between solar activity and NLC altitude based on published model simulations.     

非均质壁面对液滴俘获能力的数值模拟研究

为研究不同非均质壁面对液滴的俘获能力,采用界面追踪法（FTM）结合广义滑移边界建立了接触角模型,对液滴在非均匀润湿的非均质壁面上的运动过程进行了数值模拟研究。液滴在倾斜壁面上受到重力作用由均匀润湿部分下滑至非均匀润湿部分,通过改变Bo数、Oh数、非均匀润湿程度研究了液滴在非均匀润湿区域的运动规律。研究表明:Bo数越大,液滴运动受壁面阻力影响越小,液滴下滑的速度越快,液滴越难以被俘获;Oh数越大,液滴运动受壁面阻力影响越小,液滴越难以被俘获;非均匀润湿程度越大,非均质壁面对液滴的阻力越大,液滴越易被俘获。