Anomalous Cosmic Rays and Solar Modulation

We review aspects of anomalous cosmic rays (ACRs) that bear on the solar modulation of energetic particles in the heliosphere. We show that the latitudinal and radial gradients of these particles exhibit a 22-year periodicity in concert with the reversal of the Sun's magnetic field. The power-law index of the low energy portion of the energy spectrum of ACRs at the shock in 1996 appears to be -1.3, suggesting that the strength of the solar wind termination shock at the helioequatorial plane is relatively weak, with s 2.8. The rigidity dependence of the perpendicular interplanetary mean free path in the outer heliosphere for particles with rigidities between 0.2 and 0.7 GV varies approximately as R2, where R is particle rigidity. There is evidence that ACR oxygen is primarily multiply charged above 20 MeV/nuc and primarily singly-charged below 16 MeV/nuc. The location of the termination shock was at 65 AU in 1987 and 85 AU in 1994.     

新型太阳能利用装置的研究

对目前太阳能的几种常见的应用领域及相关装置进行了分析和研究,并在此基础上,结合相关理论,设计了利用太阳能的新型装置,如:太阳能房、太阳能热发电装置、聚光式太阳能电池发电装置等,这些装置将为更好地利用太阳能开辟新的途径.太阳能作为一种新兴的可再生能源有着不可限量的发展前景.     

Deep Impact: A Large-Scale Active Experiment on a Cometary Nucleus

The Deep Impact mission will provide the first data on the interior of a cometary nucleus and a comparison of those data with data on the surface. Two spacecraft, an impactor and a flyby spacecraft, will arrive at comet 9P/Tempel 1 on 4 July 2005 to create and observe the formation and final properties of a large crater that is predicted to be approximately 30-m deep with the dimensions of a football stadium. The flyby and impactor instruments will yield images and near infrared spectra (1–5 μm) of the surface at unprecedented spatial resolutions both before and after the impact of a 350-kg spacecraft at 10.2 km/s. These data will provide unique information on the structure of the nucleus near the surface and its chemical composition. They will also used to interpret the evolutionary effects on remote sensing data and will indicate how those data can be used to better constrain conditions in the early solar system.     

Influence of the Solar Cycle on the General Circulation of the Stratosphere and Upper Troposphere

The record of dynamical structure reveals a systematic variation that operates coherently with the 11-yr variation of UV irradiance. Involving periods shorter than 5 years, the systematic variation reflects the influence of the QBO on the polar-night vortex. It has the same basic structure as interannual changes associated with the residual mean circulation of the stratosphere. A signature of the solar cycle also appears in the direct correlation to solar flux, as recovered through regression of the entire monthly record. That signature, however, is sharply enhanced around solstice, when the residual circulation is active, and during extremal phases of the QBO. In the tropics, the solar signature follows, throughout the year, from a decadal modulation in the frequency of the QBO. The modulation is manifested to either side of the QBO’s mean frequency, in two spectral peaks where the QBO dwells: one at (24 months)⁻¹, reflecting a Biennial Oscillation (BO), and another at (36 months)^-1. Intrinsic to the QBO, those peaks are separated from its mean frequency by ∼11 years⁻¹.Through the QBO’s residual circulation, the decadal modulation introduces anomalies in the subtropics, with symmetry about the equator. Accompanying anomalous temperature in the subtropics is a stronger signature over the winter pole. Discovered by Labitzke and van Loon 1988, that solar signature reflects anomalous downwelling of the Brewer-Dobson circulation. It is shown to follow through the BO, which is intrinsic to the QBO and its modulation of the polar-night vortex.     

Composition of Light Solar Wind Noble Gases in the Bulk Metallic Glass flown on the Genesis Mission

We discuss data of light noble gases from the solar wind implanted into a metallic glass target flown on the Genesis mission. Helium and neon isotopic compositions of the bulk solar wind trapped in this target during 887 days of exposure to the solar wind do not deviate significantly from the values in foils of the Apollo Solar Wind Composition experiments, which have been exposed for hours to days. In general, the depth profile of the Ne isotopic composition is similar to those often found in lunar soils, and essentially very well reproduced by ion-implantation modelling, adopting the measured velocity distribution of solar particles during the Genesis exposure and assuming a uniform isotopic composition of solar wind neon. The results confirm that contributions from high-energy particles to the solar wind fluence are negligible, which is consistent with in-situ observations. This makes the enigmatic “SEP-Ne” component, apparently present in lunar grains at relatively large depth, obsolete. ²⁰Ne/ ²²Ne ratios in gas trapped very near the metallic glass surface are up to 10% higher than predicted by ion implantation simulations. We attribute this superficially trapped gas to very low-speed, current-sheet-related solar wind, which has been fractionated in the corona due to inefficient Coulomb drag.     

Multidecadal Signal of Solar Variability in the Upper Troposphere During the 20th Century

Studies based on data from the past 25–45 years show that irradiance changes related to the 11-yr solar cycle affect the circulation of the upper troposphere in the subtropics and midlatitudes. The signal has been interpreted as a northward displacement of the subtropical jet and the Ferrel cell with increasing solar irradiance. In model studies on the 11-yr solar signal this could be related to a weakening and at the same time broadening of the Hadley circulation initiated by stratospheric ozone anomalies. Other studies, focusing on the direct thermal effect at the Earth’s surface on multidecadal scales, suggest a strengthening of the Hadley circulation induced by an increased equator-to-pole temperature gradient. In this paper we analyse the solar signal in the upper troposphere since 1922, using statistical reconstructions based on historical upper-air data. This allows us to address the multidecadal variability of solar irradiance, which was supposedly large in the first part of the 20th century. Using a simple regression model we find a consistent signal on the 11-yr time scale which fits well with studies based on later data. We also find a significant multidecadal signal that is similar to the 11-yr signal, but somewhat stronger. We interpret this signal as a poleward shift of the subtropical jet and the Ferrel cell. Comparing the magnitude of the two signals could provide important information on the feedback mechanisms involved in the solar climate relationship with respect to the Hadley and Ferrel circulations. However, in view of the uncertainty in the solar irradiance reconstructions, such interpretations are not currently possible.     

Propagation of interplanetary shocks into the Earth’s magnetosphere

This paper is devoted to the study of propagation of disturbances caused by interplanetary shocks (IPS) through the Earth’s magnetosphere. Using simultaneous observations of various fast forward shocks by different satellites in the solar wind, magnetosheath and magnetosphere from 1995 till 2002, we traced the interplanetary shocks into the Earth’s magnetosphere, we calculated the velocity of their propagation into the Earth’s magnetosphere and analyzed fronts of the disturbances. From the onset of disturbances at different satellites in the magnetosphere we obtained speed values ranging from 500 to 1300 km/s in the direction along the IP shock normal, that is in a general agreement with results of previous numerical MHD simulations. The paper discusses in detail a sequence of two events on November 9th, 2002. For the two cases we estimated the propagation speed of the IP shock caused disturbance between the dayside and nightside magnetosphere to be 590 km/s and 714–741 km/s, respectively. We partially attributed this increase to higher Alfven speed in the outer magnetosphere due to the compression of the magnetosphere as a consequence of the first event, and partially to the faster and stronger driving interplanetary shock. High-time resolution GOES magnetic field data revealed a complex structure of the compressional wave fronts at the dayside geosynchronous orbit during these events, with initial very steep parts (10 s). We discuss a few possible mechanisms of such steep front formation in the paper.     

基于驱动机构作动的太阳翼振动控制原理与实验研究

针对航天器在调姿或变轨过程中太阳翼长时间、低频振动引起航天器系统无法正常工作的问题,以太阳翼自身驱动机构为作动器,提供反馈控制力,进行振动抑制。在原理性研究的基础上,建立了贴近工程实际的真实尺寸太阳翼有限元模型,改进了控制算法,实现了太阳翼在振动控制结束后的正确复位,并利用动力学缩比模型对振动抑制方法的有效性开展了实验验证。结果表明:该方法不需引入额外的非有效载荷,能够在保证太阳翼不偏离目标位置的同时,有效抑制太阳翼的低频振动。     

航天器柔性太阳翼最优PPF主动振动抑制方法

针对采用可变速控制力矩陀螺(VSCMG)进行柔性太阳翼振动抑制问题,提出一种基于求解非光滑 H∞ 综合问题的最优参数正位置反馈(PPF)控制方法。首先,建立考虑VSCMG和柔性太阳翼耦合的振动模型,得到了线性化的约束陀螺柔性板动力学模型,基于同位控制思想推导了以角度陀螺为测量装置的约束陀螺柔性板全阶状态空间模型。针对被控对象特性,确定最优PPF控制器的结构构型和待优化参数。进而,通过对约束陀螺柔性板全阶状态空间模型进行降阶、修正和加权处理,将PPF控制器参数优化问题转化为在PPF控制器构型约束条件下的非光滑H∞综合问题,并应用一阶下降算法进行寻优求解,实现最优PPF控制器的设计。该方法能够实现对各阶陀螺模态的独立控制,在保证快速性和鲁棒性的前提下,实现最优PPF参数的稳定高效求解。仿真结果表明,所提出的最优PPF控制方法能够快速、鲁棒地实现航天器柔性太阳翼的主动振动抑制。     

InxGa1-xAs材料在多结空间太阳电池中的应用进展

In_xGa_(1-x)As材料具有独特的物理特性,可以通过调节In和Ga的组分来改变材料的带隙宽度Eg。该材料自进入多结空间太阳电池领域以来,就受到了广泛的关注。因此,In_xGa_(1-x)As材料有望成为未来多结空间太阳电池领域中的重要研究对象。本文首先介绍了InGaAs材料的生长工艺及其在多结空间太阳电池领域中的应用情况和研究现状,同时讨论了材料的外延生长工艺以获得高质量含InGaAs材料的多结太阳电池。此外,介绍了近年来InGaAs材料在高效多结空间太阳电池领域的研究进展,并对其抗辐照性能进行了简述。大量研究表明:InGaAs材料的使用可以进一步提升多结空间太阳电池的光电转换效率,达到提升卫星有效载荷的目的。