Long-Term Fluences of Solar Energetic Particles from H to Fe

Data from ACE and GOES have been used to measure Solar Energetic Particle (SEP) fluence spectra for H, He, O, and Fe, over the period from October 1997 to December 2005. The measurements were made by four instruments on ACE and the EPS sensor on three GOES satellites and extend in energy from ∼0.1 MeV/nuc to ∼100 MeV/nuc. Fluence spectra for each species were fit by conventional forms and used to investigate how the intensities, composition, and spectral shapes vary from year to year.     

基于视线矢量的深空自主导航算法研究

针对深空探测器在行星际飞行的轨道确定问题, 研究了一种基于视线矢量的自主导航算法. 结合深空探测任务的特点, 以太阳视线矢量和地球视线矢量作为导航系统的观测量, 在详细分析太阳敏感器测量原理的基础上, 给出了太阳视线矢量的观测模型及其观测误差表达式. 通过分析导航相机观测原理, 给出像元像线观测模型, 并推导了地球视线矢量的观测误差. 根据惯性空间内视线矢量间的几何关系, 详细推导了探测器的位置矢量及其误差表达式, 结合非线性扩展卡尔曼滤波建立自主导航算法. 利用深度撞击任务的实际飞行数据对本文提出的深空自主导航算法进行了仿真验证.      

协同制导导引头最大指向角误差分析

在协同制导条件下,建立了导引头最大预定指向角误差模型,分析了各种因素对协同制导条件下导引头最大预定指向角误差的影响。结果表明,雷达测角误差和系统时延是影响协同制导中末交班导引头最大指向角误差的主要因素。     

Study of the solar Slow Sonic,Alfvén and Fast Magnetosonic transition surfaces

In this paper we study the shape, extend and time variations of the solar wind transition surfaces using the Lima and Priest (1993) hydrodynamic model adequately adapted for the case of the solar wind flow. The transition surfaces, namely the Slow (Sonic), the Alfvén, and the Fast Magnetosonic surface, are important boundaries around the Sun and play a crucial role in the development of the solar wind and the structure of the inner heliosphere. We determine the shape and dimension of these surfaces as a function of heliographic latitude using measurements from Ulysses spacecraft, and we also study their temporal variation using data from spacecrafts at 1 AU (OMNI database). Furthermore, we establish their dependence with the solar activity, demonstrating their shape and location for the last two solar cycles. From this we noticed that the temporal variation of all transition surfaces follows the 11-year solar cycle. Finally, from the OMNI database, we have studied the temporal variation over the past 40 years of the plasma β parameter, the kinetic to magnetic and the kinetic to thermal energy ratios, at a distance of 1 AU from the Sun.     

The dynamic chromosphere: Pushing the boundaries of observations and models

The interface between the bright solar surface and the million-degree corona continues to hold the key to many unsolved problems in solar physics. Advances in instrumentation now allow us to observe the dynamic structures of the solar chromosphere down to less than $0_{.}^{″}1$ with cadences of just a few seconds and in multiple polarisation states. Such observational progress has been matched by the ever-increasing sophistication of numerical models, which have become necessary to interpret the complex observations. With an emphasis on the quiet Sun, I will review recent progress in the observation and modelling of the chromosphere. Models have come a long way from 1D static atmospheres, but their predictions still fail to reproduce several key observed features. Nevertheless, they have given us invaluable insight into the physical processes that energise the atmosphere. With more physics being added to models, the gap between predictions and observations is narrowing. With the next generation of solar observatories just around the corner, the big question is: will they close the gap?     

Testing the asymmetric cone model for halo CMEs using STEREO/SECCHI coronagraphic observations

Space weather is significantly controlled by halo coronal mass ejections (HCMEs) originating close to the central meridian and directing toward the Earth. Unfortunately, coronagraphic observations (especially for HCMEs) are subject to a projection effect which makes it impossible to determine the true radial velocity and width of CMEs. However, these parameters can be estimated by correcting for the projection effect using the asymmetric cone model (Michalek, 2006). A set of 20 CMEs, observed as halo events in the LASCO field of view and simultaneously as limb events in the STEREO/SECCHI field of view, are used to check the accuracy of the asymmetric cone model. For this purpose, characteristics of the considered CMEs (angular widths and radial speeds) measured in STEREO/SECCHI images are compared with those obtained by the asymmetric cone model. We demonstrate that the widths and speeds determined by both methods are very similar. Correlation coefficients for speeds and angular widths are 0.99 and 0.96, respectively. We have also shown that the projection effect is unpredictable and could sometimes be very significant (up to 100% of the velocity measured in the LASCO field of view). On average, the SOHO/LASCO projected speeds for the HCMEs are 23% smaller than the radial velocities obtained from the STEREO/SECCHI images.     

Maneuver planning of a rigid spacecraft with two skew control moment gyros

The attitude maneuver planning of a rigid spacecraft using two skew single-gimbal control moment gyros (CMGs) is investigated. First, two types of restrictions are enforced on the gimbal motions of two skew CMGs, with each restriction yielding continuous control torque along a principal axis of the spacecraft. Then, it is proved that any axis fixed to the spacecraft can be pointed along an arbitrary inertial direction by at most two sequent rotations around the two actuated axes. Given this fact, a two-step eigenaxis rotation strategy, executing by the two single-axis torques respectively, is designed to point a given body-fixed axis along a desired direction. Furthermore, a three-step eigenaxis rotation strategy is constructed to achieve an arbitrary rest-to-rest attitude maneuver. The rotation angles required for the single-axis pointing and arbitrary attitude maneuver schemes are all analytically solved. Numerical examples are presented to demonstrate the effectiveness of the proposed algorithms.     

随机馈相法对相控阵天线增益和指向精度的影响

分别以2位和3位数字移相器为例,研究了四舍五入法、适当随机量化法和预加相位法等3种随机馈相法,对均匀微带直线阵列的增益方向图和波束指向精度的影响,研究证明相对于四舍五入馈相方法,适当随机量化法和预加相位法能够极大地提高波束指向精度,但是在移相器位数较少的情况下增益会有少许损失。研究结果可为大型相控阵天线的设计提供参考。     

耦合运动对星间激光链路瞄准过程影响及补偿方法研究

在星间激光链路的瞄准过程中,光通信终端与卫星平台的耦合运动是影响瞄准精度的重要因素。本文以耦合运动数学模型为基础,建立了仿真实验系统,并以铱星系统为例,对低轨卫星星间激光链路光束瞄准过程进行了仿真研究。理论分析和仿真结果表明,终端与平台耦合运动所产生的瞄准偏差大于0.9mrad,目标卫星可接收到的信标光功率将被衰减达-7.2dB以上,严重影响目标卫星对信标光的捕获。为确保星间激光链路的建立,提出了耦合运动补偿方法,并进行了相应的仿真实验。仿真结果表明,补偿控制方法使耦合运动产生的瞄准偏差小于2μrad,对信标光的衰减小于-1.7×10-5dB,衰减量可忽略不计。该结果对低轨卫星间激光组网技术的研究具有重要意义。     

卫星光通信终端二维转台运动参量对天线指向影响研究

二维转台与卫星平台间的耦合运动，是影响卫星光通信终端天线指向控制的重要因素。在耦合动力学模型基础上，研究了二维转台不同运动参量对光通信终端天线指向偏差的影响。分析结果表明：在耦合动力学环境下，光束指向偏差随二维转台转动成规律性变化；当方位轴、俯仰轴转角θh、θv分别为（π，0）、（-π，0）时，指向偏差出现最大值；随二维转台转动时间的增加，天线指向偏差略有增加，转动时间由10s增加到1000s时增幅仅为1％。其结果为补偿耦合运动影响，保证天线指向控制精度，提高卫星光通信终端星上应用的稳定性打下基础。