中国及邻近地区地磁场垂直梯度的计算与研究

根据地磁场的球谐模型,推导出地磁场各个分量垂直梯度的球谐表达式.计算出中国及邻近地区高度为0km,50km和100km处的地磁场及其垂直梯度的网点值,编绘出地磁总强度、垂直强度、水平强度和磁偏角的垂直梯度等值线图.研究了地磁场垂直梯度在地面上以及随高度的变化规律.     

Prediction tests by using “ISF” method for the geomagnetic disturbances

A so-called “ISF” prediction method for geomagnetic disturbances caused by solar wind storms blowing to the Earth is suggested. The method is based on a combined approach of solar activity, interplanetary scintillation (I) and geomagnetic disturbance observations during the period 1966–1982 together with the dynamics of solar wind storm propagation (S) and fuzzy mathematics (F). It has been used for prediction tests for 37 geomagnetic disturbance events during the descending solar activity phase 1984–1985, and was presented in 33rd COSPAR conference. Here, it has been improved by consideration of the three dimensional propagation characteristics of each event, the search for the best radio source and the influence of the southward components of interplanetary magnetic fields on the geomagnetic disturbances. It is used for prediction tests for 24 larger geomagnetic disturbance events that produced space anomalies during the period 1980–1999. The main results are: (1) for the onset time of the geomagnetic disturbance, the relative error between the observation, T_obs, and the prediction, T_pred, ΔT_pred/T_obs  10% for 45.8% of all events, 30% for 78.3% and >30% for only 21.7%; (2) for the magnetic disturbance magnitude, the relative error between the observation, ∑K_p,obs, and the prediction, ∑K_p,pred, Δ∑K_p,pred/∑K_p,obs  10% for 41.6% of all events, 30% for 79% and 45% for 100%. This shows that the prediction method described here has encouraging prospects for improving predictions of large geomagnetic disturbances in space weather events.     

基于星载加速度计反演载人航天轨道大气密度

热层大气密度直接影响低轨道航天器的精密定轨,热层大气密度模型的误差是影响载人航天定轨精度的关键因素。选取400km为载人航天轨道的代表高度,利用CHAMP卫星数据修正热层大气密度模型,进而反演得到2002年的热层大气密度,统计其中长期变化特征,并分析大气密度与太阳活动和地磁活动的关系,得出热层大气密度与两种指数的总体变化趋势一致的结论,且地磁活动与大气密度的相关性更好。同时将大气密度的反演值与神舟三号飞船的实测密度值进行对比,结果显示二者有较好的一致性,其平均残差和均方根误差分别为0．03和0．24,并且地磁平静期的误差明显小于磁暴期。结果表明,利用星载加速度计数据反演载人航天轨道大气密度是一种有效的方法。     

多视场低磁星敏感器及其在磁测卫星中的应用

下一代地磁导航等空间任务对地球磁场测量卫星提出了迫切的需求, 高精度地磁场测量卫星需要极高的姿态测量精度和空间剩磁环境, 对星敏感器提出了新的要求。针对这一需求, 研究了低剩磁高精度星敏感器的改进设计方法。采用三视场分体结构设计,提高了数据更新率,通过数据融合提高了姿态确定精度,同时对光学头部进行了精细化降剩磁设计。仿真和测试结果表明,改进的星敏感器设计方法能够实现较低的剩磁和较高的定姿精度, 满足地磁场测量卫星的应用需求, 具有较高的应用价值。     

Some effects in the upper atmosphere during geomagnetic storms

This paper examines the response of the high latitude ionosphere–thermosphere system during two intense geomagnetic storms. For that, data taken by instruments on board Dynamic Explorer 2 taken at heights of the F2-layer are used. These results represent a comparison of simultaneous measurements of storm disturbances in gas composition, electron density and temperature in common local time sectors. Documented are an increase in electron temperature and a decrease in electron density; increases both in electron temperature and electron density; and the correlation between electron density decreases and increases in the ratio N₂/O. It is noticed that the decrease in electron density is sometimes due to an increase in the molecular nitrogen density N₂ and not always is attributed both to the increase in N₂ density and the simultaneous decrease in the atomic oxygen density.     

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.     

Dynamical Simulations of Plasmapause Deformations

Dynamical simulations have been developed at IASB-BIRA to model the deformations of the plasmasphere during geomagnetic substorms and other variations in the level of geomagnetic activity. The simulations are based on the mechanism of plasma instability and use the empirical Kp-dependent electric field E5D. The results of the simulations are compared with IMAGE observations that provide the first global comprehensive images of the Earth’s plasmasphere. The predicted plasmapause positions correspond generally rather satisfactorily with the EUV observations. The plasmasphere is rather extended in all MLT sectors during quiet periods. During or just after geomagnetic substorms, the plasmaspause is sharper and becomes closer to the Earth in the night sector. Periods of enhanced geomagnetic activity are associated to the formation of plumes that rotate with the plasmasphere. The simulations reproduce the formation and the motion of these plumes, as well as the development of other structures like shoulders observed at the plasmapause by EUV on IMAGE.     

地磁导航技术研究进展

地磁场是地球的固有资源,利用地磁场匹配进行导航是一种新型导航技术.与传统的惯性导航和卫星导航比较,地磁导航具有无积累误差、抗干扰、隐蔽性好、导航信息丰富等优势.文章介绍了地磁导航的3个基本要素,即磁场测量技术、地磁模型以及定位与导航技术.分析了弱磁场磁力仪在地磁导航中的应用及其优缺点,讨论了地磁场模型和地磁匹配算法,展望了地磁导航技术的应用前景.     

基于UKF的高动态飞行器无源组合导航系统研究

针对飞行器在进行高动态飞行中卫星导航系统易受干扰、GPS可能被屏蔽,从而导致导航系统失稳甚至发散的问题,采用无迹卡尔曼滤波(UKF)算法对基于捷联惯导系统(SINS)、地磁导航系统(GNS)和嵌入式大气数据系统(FADS)的组合无源导航系统性能进行了改进.建立了地磁数据模型和无源组合导航模型,并针对新的组合导航系统观测方程非线性程度较高问题,提出了利用非线性UKF对导航数据进行融合的方法.利用高动态飞行轨迹对所提出的组合导航系统进行了仿真及误差分析,结果表明该系统对SINS误差估计具有适中的精度.     

Ionospheric F-region response to geomagnetic disturbances

The F2-region reaction to geomagnetic storms usually called as an ionospheric storm is a rather complicated event. It consists of so called positive and negative phases, which have very complicated spatial and temporal behavior. The main morphological features of ionospheric storms and the main processes governing their behavior were understood at the end of the 1900s and described in a series of review papers. During the recent decade there were many publications dedicated to the problem of ionospheric storms. In this paper a concept of ionospheric storm morphology and physics formulated at the end of the 1990s is briefly summarized and the most interesting results obtained in the 2000s are described. It is shown that the main features of the studies of the previous decade were: the use of GPS TEC data for analyzing the ionospheric storm morphology, attraction of sophisticated theoretical models for studying the processes governing ionospheric behavior in disturbed conditions, and accent to analysis of ionospheric behavior during prominent events (very strong and great geomagnetic storms). Also a special attention was paid to the pre-storm enhancements in foF2 and TEC.