一种激光多普勒测速仪辅助捷联惯导在线标定方法

针对惯组长期贮存过程中陀螺和加速度计零偏漂移的问题, 提出了一种利 用激光多普勒测速仪辅助捷联惯导的在线标定方案。给出了包括激光多普勒测速仪安装 误差角和惯组安装误差角的航位推算误差方程。基于航位推算误差方程建立了闭环卡尔 曼滤波器,对惯组零偏误差、激光多普勒测速仪安装误差角和惯组方位安装误差角进行 在线标定。仿真结果表明,加速后激光多普勒测速仪安装误差角和惯组方位安装误差角 得到估计;方位角改变后惯组零偏误差也得到估计。该方法允许跑车前不用综合标定, 直接装订前一次的安装角参数,缩短了准备时间。     

The modulation of cosmic rays in the high latitude heliosphere: A computer simulation

Modulation models based on the numerical solution of Parker's transport equation for galactic cosmic rays in the heliosphere make clear predictions about modulation in the high latitude heliosphere. However, for these predictions certain assumptions have to be made, for example, what the heliospheric magnetic field (HMF) looks like above the solar poles and what the spatial dependence of the diffusion coefficients are. For this presentation the general predictions of a standard drift model for the modulation of cosmic rays in the high latitude heliosphere, in particular predictions for the Ulysses trajectory, are discussed and critically reviewed. Preliminary results from Ulysses show a significant increase in the solar wind speed towards higher latitudes. The effects of this strong latitudinal dependence together with different modifications of the HMF at these high latitudes on the apparently too large diffusion and drifts predicted by current models are also shown.     

Time-Dependent 2d Model Compared with Observations During the 1974 Mini Cycle

The 1974 mini-cycle is a medium term cosmic ray modulation event with about one year duration. It occurred in an A>0 epoch of solar magnetic polarity during conditions of low activity, but with an increase in the latitudinal extent of the heliospheric current sheet (tilt angle α) and the magnitude B of the heliospheric magnetic field. This cosmic ray decrease can be used to test the hypothesis that such large scale decreases (mini cycles) may be caused primarily by a combination of changes in α and B. For this purpose a fully time-dependent 2D model of solar modulation is used, which includes the effects of global and current sheet drifts, and anisotropic perpendicular diffusion. Such models have been used successfully to describe the proton energy spectrum as well as the radial and latitudinal gradients near 1 AU. Comparison of the model solutions with the observed decrease for 1.8 GV protons allows us to study the combined influence of variable drift and diffusion effects throughout the event. This revised version was published online in August 2006 with corrections to the Cover Date.     

Cosmic-Ray Modulation in the Heliosphere A Phenomenological Study

The heliospheric cosmic-ray network–Pioneer 10/11, Voyager 1/2, Ulysses and IMP 8 have provided detailed observations of galactic and anomalous cosmic rays over a period of time that now exceeds 25 years and extends to heliocentric distances beyond 65 AU. These data, when compared over consecutive 11 year solar cycles, clearly establishes the existence of a 22-year cosmic ray modulation cycle that is dominated by the 11-year solar activity cycle but is strongly influenced by gradient and curvature drifts in association with the tilt of the heliospheric neutral current sheet as well as the mediation of the enhanced magnetic turbulence above the solar poles. Over successive solar minima these effects manifest themselves in the remarkable differences in the energetic particle time histories, in the magnitude and sign of the radial and latitudinal intensity gradients and in the changes in the energy spectra of anomalous cosmic rays as a function of heliocentric distance.From solar minimum to solar maximum the long term modulation is principally a combination of two solar related phenomena, the cumulative effect of long-lived global merged interaction regions (GMIRs) and gradient and curvature drifts in the interplanetary magnetic field. For the periods when positive ions flow in over the solar poles and out along the heliospheric current sheet, the modulation of ions is dominated by GMIRs. When this flow pattern is reversed it is found that drifts are an important but not dominant factor for cosmic ray modulation with the current sheet related drift effects decreasing with increasing rigidity R, heliolatitude and heliocentric distance. Over a single solar cycle these conclusions are confirmed at 1 AU by comparing the relative modulation of cosmic-ray helium nuclei and electrons.     

Cosmic Rays in the Inner Heliosphere: Insights from Observations, Theory and Models

The global modulation of galactic cosmic rays in the inner heliosphere is determined by four major mechanisms: convection, diffusion, particle drifts (gradient, curvature and current sheet drifts), and adiabatic energy losses. When these processes combine to produce modulation, the complexity increases significantly especially when one wants to describe how they evolve spatially in all three dimensions throughout the heliosphere, and with time, as a function of solar activity over at least 22 years. In this context also the global structure and features of the solar wind, the heliospheric magnetic field, the wavy current sheet, and of the heliosphere and its interface with the interstellar medium, play important roles. Space missions have contributed significantly to our knowledge during the past decade. In the inner heliosphere, Ulysses and several other missions have contributed to establish the relative importance of these major mechanisms, leading to renewed interest in developing more sophisticated theories and numerical models to explain these observations, and to understand the underlying physics that determines galactic cosmic ray modulation at Earth. An overview is given of some of the observational and modeling highlights over the past decade.     

Theory and Modeling of Galactic Cosmic Rays: Trends and Prospects

We address past and future trends in the theory and modeling of galactic cosmic rays in the heliosphere, and select some of the outstanding issues where future progress is anticipated. We discuss the theory of diffusive transport, briefly discuss drifts, the force-field approximation, and current numerical methods. Special attention is given to the areas of modeling cosmic rays in the heliosheath, the implications of the recent unusual solar minimum, and the understanding of high rigidity cosmic-ray anisotropies.     

IDENTIFICATION OF GYRO DRIFTS UNDER THREE AXIS ATTITUDE COUPLING

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箱梁颤振过程中旋涡的演化规律及气动力的变化特性

利用粒子图像测速技术（PIV）观测了箱梁颤振过程中模型周围流场的旋涡特征,以模型扭转振动位移作为参考信号,采用相位平均的方法研究了旋涡规律性演化对模型周期性振动的驱动作用。风速较低时,箱梁振幅很小,其尾部风嘴附近上侧的旋涡尺度也很小,不易观测到,而下侧的旋涡尺度较大,其形状接近于圆形。当风速接近颤振临界风速时,箱梁振幅明显增大,并且模型尾部风嘴上侧的旋涡尺度也显著增大,达到与下侧旋涡尺度相匹配的程度,模型尾部风嘴上下侧旋涡的交替作用主导了结构振动直到模型振动发散。基于流固松耦合的计算策略,采用计算流体动力学（CFD）的数值方法模拟了箱梁颤振临界状态下的绕流特性,结合正交特征分解（POD）的方法研究了模型颤振时刻表面压力的空间分布特征,通过分析发现在颤振过程中箱梁表面波动压力的主控成分向迎风侧风嘴漂移。     

New Insights on Geomagnetic Storms from Model Simulations Using Multi-Spacecraft Data

The forecast of the terrestrial ring current as a major contributor to the stormtime Dst index and a predictor of geomagnetic storms is of central interest to ‘space weather’ programs. We thus discuss the dynamical coupling of the solar wind to the Earth's magnetosphere during several geomagnetic storms using our ring current-atmosphere interactions model and coordinated space-borne data sets. Our model calculates the temporal and spatial evolution of H⁺, O⁺, and He⁺ ion distribution functions considering time-dependent inflow from the magnetotail, adiabatic drifts, and outflow from the dayside magnetopause. Losses due to charge exchange, Coulomb collisions, and scattering by EMIC waves are included as well. As initial and boundary conditions we use complementary data sets from spacecraft located at key regions in the inner magnetosphere, Polar and the geosynchronous LANL satellites. We present recent model simulations of the stormtime ring current energization due to the enhanced large-scale convection electric field, which show the transition from an asymmetric to a symmetric ring current during the storm and challenge the standard theories of (a) substorm-driven, and (b) symmetric ring current. Near minimum Dst there is a factor of ∼ 10 variation in the intensity of the dominant ring current ion specie with magnetic local time, its energy density reaching maximum in the premidnight to postmidnight region. We find that the O⁺ content of the ring current increases after interplanetary shocks and reaches largest values near Dst minimum; ∼ 60% of the total ring current energy was carried by O⁺ during the main phase of the 15 July 2000 storm. The effects of magnetospheric convection and losses due to collisions and wave-particle interactions on the global ring current energy balance are calculated during different storm phases and intercompared. This revised version was published online in August 2006 with corrections to the Cover Date.     

高精度激光陀螺仪温度补偿模型研究

在实际工程中,高精度激光陀螺仪的输出零偏会随着温度变化发生漂移,限制了其应用。为了降低和补偿温度对陀螺零偏的影响,提高陀螺应用性能,降低装备成本,从探究温度对输出零偏的影响因素出发,建立了一种考虑多影响因素的温度补偿模型,并设计了相应的温度试验。试验结果表明,高精度机抖激光陀螺的零偏和温度、温变速率、温度梯度具有较好的相关性和重复性,该温度补偿模型补偿效果显著,可基本消除零偏随温度变化的趋势,有效降低武器装备对零部件的要求,能够降低应用成本,具有很强的实用价值。     

Polar rain entry of galactic electrons into the inner heliosphere?

The understanding of the relative intensity variations in cosmic ray ions and electrons with respect to solar modulation is a grand challenge for cosmic ray modulation theory. Although effects of the heliospheric neutral sheet, gradient-curvature drifts, and merged interaction regions provide qualitative explanations for observed solar cycle variations of high energy protons and ions, these effects do not account for the anomalously high intensities of high energy galactic electrons at 22-year intervals of the solar magnetic solar cycle. From the similar modulation responses of protons and heavy ions it does not appear that cosmic ray pressure effects, dominated by protons, can account for the chargesign asymmetry of cosmic ray modulation. External factors including modulation in the heliosheath and polar linkage to the interstellar magnetic field are examined as potential causes of symmetry breaking for electron modulation with respect to the solar magnetic polarity at solar minimum.     

Interlaced optimal-REQUEST and unscented Kalman filtering for attitude determination

 Aimed at low accuracy of attitude determination because of using low-cost components which may result in non-linearity in integrated attitude determination systems, a novel attitude determination algorithm using vector observations and gyro measurements is presented. The various features of the unscented Kalman filter (UKF) and optimal-REQUEST (quaternion estimator) algorithms are introduced for attitude determination. An interlaced filtering method is presented for the attitude determination of nano-spacecraft by setting the quaternion as the attitude representation, using the UKF and optimal-REQUEST to estimate the gyro drifts and the quaternion, respectively. The optimal-REQUEST and UKF are not isolated from each other. When the optimal-REQUEST algorithm estimates the attitude quaternion, the gyro drifts are estimated by the UKF algorithm synchronously by using the estimated attitude quaternion. Furthermore, the speed of attitude determination is improved by setting the state dimension to three. Experimental results show that the presented method has higher performance in attitude determination compared to the UKF algorithm and the traditional interlaced filtering method and can estimate the gyro drifts quickly.     

Analytical long-term evolution and perturbation compensation models for BeiDou MEO satellites

The current paper establishes the analytical models of the long-term evolution and perturbation compensation strategy for Medium Earth Orbits(MEO)shallow-resonant navigation constellation,with application to the Chinese Bei Dou Navigation Satellite System(BDS).The long-term perturbation model for the relative motion is developed based on the Hamiltonian model,and the long-term evolution law is analyzed.The relationship between the control boundary of the constellation and the offset of the orbital elements is analyzed,and a general analytical method for calculating the offset of the orbit elements is proposed.The analytical model is further improved when the luni-solar perturbations are included.The long-term evolutions of the BDS MEO constellation within 10 years are illustrated,and the effectiveness of the proposed analytical perturbation compensation calculation approach is compared with the traditional numerical results.We found the fundamental reason for the nonlinear variations of the relative longitude of ascending node and the mean argument of latitude is the long-periodic variations of the orbital inclination due to the luni-solar perturbations.The proposed analytical approach can avoid the numerical iterations,and reveal the essential relationship between the orbital element offsets and the secular drifts of the constellation configuration.Moreover,there is no need for maintaining the BDS MEO constellation within 10 years while using the perturbation compensation method.     

Low Latitude Ionospheric Electrodynamics

The low latitude ionosphere is strongly affected by several highly variable electrodynamic processes. Over the last two decades ground-based and satellite measurements and global numerical models have been extensively used to study the longitude-dependent climatology of low latitude electric fields and currents. These electrodynamic processes and their ionospheric effects exhibit large ranges of temporal and spatial variations during both geomagnetic quiet and disturbed conditions. Numerous recent studies have investigated the short term response of equatorial electric fields and currents to lower atmospheric transport processes and solar wind-magnetosphere driving mechanisms. This includes the large electric field and current perturbations associated with arctic sudden stratospheric warming events during geomagnetic quiet times and highly variable storm time prompt penetration and ionospheric disturbance dynamo effects. In this review, we initially describe recent experimental and numerical modeling results of the global climatology and short term variability of quiet time low latitude electrodynamic plasma drifts. Then, we examine the present understanding of equatorial electric field and current perturbation fields during periods of enhanced geomagnetic activity.     

纬度未知条件下罗经系统行进中启动方法研究

介绍了一种适用于罗经系统在无法获得纬度情况下的航行中启动方法。基于惯性坐标系下的两个不同时间段内的重力加速度积分值实现纬度估计,根据估计的纬度值,完成初始对准。在动基座条件下,通过引入辅助速度信息补偿掉由于载体机动产生的误差,从而实现行进中启动。启动后采用组合导航或纯惯性导航的方式,可以实现方位的保持。通过分析发现,纬度估计精度主要受等效北向陀螺漂移的影响,方位对准精度主要受等效东向陀螺漂移的影响;试验结果表明,在300s时间内,方位角对准精度可以达到0.1°(RMS)。     

改进的格网惯导系统无阻尼综合校正方法

综合校正技术可作为抑制格网惯导系统（INS）导航误差的有效手段。加速度计零偏所造成的水平姿态误差是导致综合校正中陀螺漂移估计精度受限的重要因素。针对这一问题，提出了一种改进的无阻尼综合校正方法。首先，推导了格网坐标系框架下估计加速度计零偏和姿态的目标函数；其次，介绍了无阻尼条件下综合校正的两个核心方程；最后设计了无阻尼两点校策略。综合校正前，在多普勒计程仪（DVL）提供的速度辅助下完成加速度计零偏的估计和补偿，以此消除加速度计零偏所造成的水平姿态误差对综合校正中陀螺漂移估计精度的影响。在两次间断的外部位置和航向辅助下通过所设计的综合校正策略完成对陀螺漂移的估计。校正策略中所涉及的水平姿态误差在DVL辅助下由参数估计方法估计得到。仿真及实验结果表明：与现有的研究相比，所设计的综合校正方案进一步减少了DVL的辅助时间，同时由于准确地估计和补偿了加速度计零偏，陀螺漂移的估计精度显著提高，该方案在抑制导航误差方面具备更明显的优势。     

Nonlinear dust Alfvén modes

Nonlinear modes are investigated in magnetized dusty plasmas, where the dust dynamics is modelled by a number of cold, highly negatively charged and very massive fluids, besides ordinary electrons and protons. Several low-frequency motions occur which are typical for the dust components, some of them described by model equations such as the derivative nonlinear Schrödinger equation for electromagnetic waves. One can include equilibrium drifts and even fluctuations in the grain charges. Most of the preceding conclusions are relevant for different kinds of astrophysical and heliospheric plasmas.     

Confronting Observations and Modeling: The Role of the Interstellar Magnetic Field in Voyager 1 and 2 Asymmetries

Magnetic effects are ubiquitous and known to be crucial in space physics and astrophysical media. We have now the opportunity to probe these effects in the outer heliosphere with the two spacecraft Voyager 1 and 2. Voyager 1 crossed, in December 2004, the termination shock and is now in the heliosheath. On August 30, 2007 Voyager 2 crossed the termination shock, providing us for the first time in-situ measurements of the subsonic solar wind in the heliosheath. With the recent in-situ data from Voyager 1 and 2 the numerical models are forced to confront their models with observational data. Our recent results indicate that magnetic effects, in particular the interstellar magnetic field, are very important in the interaction between the solar system and the interstellar medium. We summarize here our recent work that shows that the interstellar magnetic field affects the symmetry of the heliosphere that can be detected by different measurements. We combined radio emission and energetic particle streaming measurements from Voyager 1 and 2 with extensive state-of-the art 3D MHD modeling, to constrain the direction of the local interstellar magnetic field. The orientation derived is a plane ～60°–90° from the galactic plane. This indicates that the field orientation differs from that of a larger scale interstellar magnetic field, thought to parallel the galactic plane. Although it may take 7–12 years for Voyager 2 to leave the heliosheath and enter the pristine interstellar medium, the subsonic flows are immediately sensitive to the shape of the heliopause. The flows measured by Voyager 2 in the heliosheath indicate that the heliopause is being distorted by local interstellar magnetic field with the same orientation as derived previously. As a result of the interstellar magnetic field the solar system is asymmetric being pushed in the southern direction. The presence of hydrogen atoms tend to symmetrize the solutions. We show that with a strong interstellar magnetic field with our most current model that includes hydrogen atoms, the asymmetries are recovered. It remains a challenge for future works with a more complete model, to explain all the observed asymmetries by V1 and V2. We comment on these results and implications of other factors not included in our present model.     

速率方位惯性导航系统

本文提出一种把平台式和捷联式惯导系统结合在一起的新的惯性导航系统。在该系统中使用的速率方位平台没有方位稳定回路、方位坐标分解器及同步器。平台和运载器的方位角是根据由水平环架支承的方位速率陀螺讯号借助积分运算得到的。这种惯导系统适用于运输机、飞航式及弹道式导弹等不作大角度俯仰机动的运载器。文中叙述了方位速率平台的工作原理、力学编排方程、初始对准的特点以及陀螺漂移的标定和补偿;同时对各主要误差源所引起的姿态、速度和导航定位误差的传播特性进行了模拟计算。在结论中指出:平台的结构简单、体积小、重量轻、可靠性好、可对方位陀螺的漂移进行标定和补偿是其独特优点。另外,如果利用专门的光学系统,配合已知地标的方位角和纬度,不仅能够实现快速对准,而且还可进行水平陀螺的标定和补偿。     

Electric Fields and Magnetic Fields in the Plasmasphere: A Perspective From CLUSTER and IMAGE

The electric field and magnetic field are basic quantities in the plasmasphere measured since the 1960s. In this review, we first recall conventional wisdom and remaining problems from ground-based whistler measurements. Then we show scientific results from Cluster and Image, which are specifically made possible by newly introduced features on these spacecraft, as follows. 1. In situ electric field measurements using artificial electron beams are successfully used to identify electric fields originating from various sources. 2. Global electric fields are derived from sequences of plasmaspheric images, revealing how the inner magnetospheric electric field responds to the southward interplanetary magnetic fields and storms/substorms. 3. Understanding of sub-auroral polarization stream (SAPS) or sub-auroral ion drifts (SAID) are advanced through analysis of a combination of magnetospheric and ionospheric measurements from Cluster, Image, and DMSP. 4. Data from multiple spacecraft have been used to estimate magnetic gradients for the first time.