冷原子干涉仪发展现状与应用分析

基于冷原子干涉仪的量子传感器具有极高的理论精度,在自然科学的各个领域特别是重力测量和惯性传感领域有着广泛的应用。首先介绍了原子干涉仪的基本原理,在此基础上给出了基于双光子受激Raman跃迁的脉冲式Mach-Zehnder原子干涉仪的干涉相位,描述了原子干涉仪在重力仪和陀螺上的应用及其发展历程,着重分析了当前发展最成熟的原子重力仪的发展历程和趋势,指出了原子干涉仪应用的发展方向。     

太阳高能粒子事件上升时间统计研究

选取1997-2006年共66个较大的缓变型太阳高能粒子(SEP)事件, 分析了不同条件下太阳高能粒子通量廓线上升时间与源区日面经向分布之间的相关关系, 研究了日冕物质抛射(CME)和耀斑在SEP上升阶段的作用特点.统计结果表明,大SEP事件的源区主要分布在太阳西半球, 特别是磁足点东西两侧45°范围内; 在高速太阳风条件下, 低能通道的通量上升时间与日面相对经度有较好的相关性,即离磁足点越远, 上升时间越长,而高能通道相关性则不明显; 全晕状CME产生的SEP事件对应的上升时间与源区位置没有明显的相关性, 而部分晕状CME伴随的SEP事件则与二次拟合曲线符合很好.分析表明,在缓变型SEP事件的通量上升阶段, 耀斑加速过程起着重要作用,这在部分晕状CME伴随的SEP事件中尤为显著.      

三相六开关VIENNA整流器功率开关开路故障诊断

分析了VIENNA整流器在桥臂各个功率器件出现开路故障时所呈现的故障特征,指出了各桥臂续流二极管的开路故障对整流器的危害最大。进一步提出了利用三相输入电流直流分量以及输出电压交流纹波作为功率器件开路故障诊断的故障特征值。构建了基于人工神经网络的功率开关开路故障分类系统,并将所提取的故障特征值作为输入训练样本对其进行训练,最后通过MATLAB软件中M语言编程完成对故障分类系统的训练和测试。训练和测试的结果表明,训练后的神经网络故障分类系统可很好地对VIENNA整流器除续流二极管外的功率器件开路故障进行定位。     

太阳高能粒子在行星际中的扩散过程

当太阳活动频繁,特别是有耀斑爆发或者日冕物质抛射驱动的激波时,经常能够观察到高能粒子(能量从几十keV到几十MeV)通量突然增加,这种由太阳活动产生的高能粒子事件被称为太阳高能粒子事件。文章研究了耀斑和日冕物质抛射产生的两类高能粒子事件,重点讨论了高能粒子横越磁力线的扩散对粒子在行星际空间传播过程中所起到的作用,给出了对于不同扩散系数条件的数值模拟结果。     

基于SAMPEX卫星观测的南大西洋异常区高能质子动态分布特征

利用SAMPEX卫星1992年7月至2004年6月19～27MeV高能质子数据对南大西洋异常区的分布特征进行研究, 发现南大西洋异常区高能质子分布随高度及F_10.7的变化十分显著. 在540±25km高度上, 地磁较为平静时期南大西洋异常区高能质子微分通量随着F_10.7的增大而减小, 同时在F_10.7≥115sfu时减小趋势较为平缓. 对中等及以上磁暴进行统计分析发现, 磁暴期间南大西洋异常区高能质子微分通量和SYM-H指数的绝对值存在明显的反相关关系, 且地磁暴对南大西洋异常区高能质子微分通量存在明显的持续影响效应. 磁暴发生期间高能质子微分通量明显减少. 磁暴恢复相及其之后高能质子微分通量呈现较为显著的恢复过程.      

用于铷原子磁光阱的超高真空系统设计

上抛式冷原子干涉重力仪,以Rb原子作为操控介质,使其在二维磁光阱中被冷却,在三维磁光阱中装载并在干涉区内实现探测。根据重力仪对真空系统的特殊要求,对真空系统的结构和参数进行设计,完成真空泵、真空腔室结构及光学玻片等关键部件的选型及设计,设计出结构紧凑实用的超高真空系统。在后期磁光阱的装配中,提出了相应的关键工艺技术,实现了超高真空系统的组装搭建。通过差分管的设计,二维磁光阱的真空度控制在10-6Pa,三维磁光阱的极限真空度达到10-8Pa。     

Performance of GPS-based accelerometry: A simulation experiment

Recent studies have shown that with the availability of high-quality CHAMP and GRACE gravity field models, it is feasible to determine accurate non-gravitational accelerations for low Earth orbiting satellites indirectly from precise GPS satellite-to-satellite observations. Possible applications of this so-called GPS-based accelerometry approach consist of accelerometer calibration and atmospheric density and wind computations. With the growing number of high-quality space-borne GPS receivers, this method could be applied to a large range of satellites. In this paper an extensive simulation study has been carried out, based on real accelerometer data from the GRACE mission, in order to determine the optimal processing strategy and the resulting accuracy of the estimated non-gravitational accelerations. It is shown that the optimal processing strategy consists of a piecewise linear parameterization of the estimated empirical accelerations, together with short 6-h orbit arcs. The GPS-based accelerometry approach makes use of triple-differenced GPS observations and the impact of considering the correlated observation noise was found to be marginal in the presence of other error sources such as GPS ephemeris errors. Using a priori non-gravitational force models improves the recovery of low temporal resolution accelerations, except during huge geomagnetic storms. With this strategy, non-gravitational accelerations can be recovered during high solar activity with an accuracy of better than 10% of the total signal in along-track direction and around 25–40% in cross-track direction, at time resolutions of around 8–20 min. During solar minimum conditions, the relative recovery error will increase to approximately 50% in along-track direction and around 60–70% in cross-track direction, due to the reduced atmospheric drag signal. Unfortunately, GPS-based accelerometry is hardly sensitive in the radial direction.     

Solar wind low-energy energetic ion enhancements: A tool to forecast large geomagnetic storms

Predicting the occurrence of large geomagnetic storms more than an hour in advance is an important, yet difficult task. Energetic ion data show enhancements in flux that herald the approach of interplanetary shocks, usually for many hours before the shock arrival. We present a technique for predicting large geomagnetic storms (Kp  7) following the arrival of interplanetary shocks at 1 AU, using low-energy energetic ions (47–65 keV) and solar wind data measured at the L1 libration point. It is based on a study of the relationship between energetic ion enhancements (EIEs) and large geomagnetic storms by Smith et al. [Smith, Z., Murtagh, W., Smithtro, C. Relationship between solar wind low-energy energetic ion enhancements and large geomagnetic storms. J. Geophys. Res. 109, A01110, 2004. doi:10.1029/ 2003JA010044] using data in the rise and maximum of solar cycle 23 (February 1998–December 2000). An excellent correlation was found between storms with Kp  7 and the peak flux of large energetic ion enhancements that almost always (93% of time in our time period) accompany the arrival of interplanetary shocks at L1. However, as there are many more large EIEs than large geomagnetic storms, other characteristics were investigated to help determine which EIEs are likely to be followed by large storms. An additional parameter, the magnitude of the post-shock total magnetic field at the L1 Lagrangian point, is introduced here. This improves the identification of the EIEs that are likely to be followed by large storms. A forecasting technique is developed and tested on the time period of the original study (the training data set). The lead times, defined as the times from the arrival of the shock to the start of the 3-h interval of maximum Kp, are also presented. They range from minutes to more than a day; the average for large storms is 7 h. These times do not include the extra warning time given when the EI flux cross the high thresholds ahead of the shock. Because the data-stream used in the original study is no longer available, we extended the original study (1998–2000) to 2001, in order to: (a) investigate EIEs in 2001; (b) present a validation of the technique on an independent data set; (c) compare the results based on the original (P1) energy channel to those of the replacement (P1′) and (d), determine new EIE thresholds for forecasting geomagnetic storms using P1′ data. The verification of this P1′ training data set is also presented, together with lead times.     

Solar proton enhancements in different energy channels and coronal mass ejections during the last solar cycle

The main properties of 11622 coronal mass ejections (CMEs) observed by the Solar and Heliospheric Observatory (SOHO) mission’s Large Angle and Spectrometric Coronagraph (LASCO-C2) from January 1996 through December 2006 are considered. Moreover, the extended database of solar proton enhancements (SPEs) with proton flux >0.1 pfu at energy >10 MeV measured at the Earth’s orbit is also studied. A comparison of these databases gives new results concerning the sources and acceleration mechanisms of solar energetic particles. Specifically, coronal mass ejections with width >180° (wide) and linear speed >800 km/s (fast) seem they have the best correlation with solar proton enhancements. The study of some specific solar parameters, such as soft X-ray flares, sunspot numbers, solar flare index etc. has showed that the soft X-ray flares with importance >M5 may provide a reasonable proxy index for the SPE production rate. From this work, it is outlined that the good relation of the fast and wide coronal mass ejections to proton enhancements seems to lead to a similar conclusion. In spite of the fact that in the case of CMEs the statistics cover only the last solar cycle, while the measurements of SXR flares are extended over three solar cycles, it is obvious for the studied period that the coronal mass ejections can also provide a good index for the solar proton production.