外辐射带动态演化的粒子模拟研究

运用计算机实验方法即三维电磁粒子模拟方法初步研究了暴时扰动情况下外辐射带粒子环境的动态演化特性。模拟计算了暴时辐射带粒子环境的演化情况。模拟计算结果显示，高能质子、电子注入午辐射滞后，两者一方面沿磁力线做弹跳运动，向高纬扩展，部分注入质子和电子沉降于南北两极区域；另一方面，注入质子和电子还经历顺时针和逆时针方向的漂移运动，粒子能量越大，漂移速度越快。暴时多次注入引起整个辐射带粒子能量的大幅增强；粒子注入颗次和强度越大，辐射带粒子通量增幅越大。本项研究为开发研制完整的辐射带动态模式积累了有益的经验。     

农林5A型飞机驾驶员座椅FAA适航验证强度分析

介绍了农5A飞机驾驶员座椅在FAA适航取证中的强度验证计算方法。先对农5A飞机驾驶员座椅验证试验假件作用在安全带和肩带上载荷进行了分析,然后施加到座椅强度有限元计算模型上进行计算。座椅经参考强度计算结果设计改进后,顺利完成了强度验证试验,满足了FAA适航要求。本文为小型飞机座椅适航取证提供了思路和方法。     

Ray Structure of the Coronal Streamer Belt and Its Manifestation as Sharp Large Peaks of Solar Wind Plasma Density at the Earth''''s Orbit

The white-light corona calibrated data with processing level L1 from the LASCO-C2/SOHO instrument, and data from the Wind spacecraft with one-hour and one-minute time resolution on quasi-stationary slow (v between 300-450 km/s at the Earth's orbit) the Solar Wind (SW) parameters in the absence of sporadic SW streams are examined. Within distances from the Sun's center less than R in the range of 20-30 Rs, (Rs, the solar radius), slow wind is known as the streamer belt, and at larger distances it is called the He-liospheric Plasma Sheet (HPS). It is shown that the streamer belt comprises a sequence of pairs of rays. In general, ray brightnesses in each pair can differ, and the magnetic field is oppositely directed in them. The neutral line of the radial magnetic field of the Sun runs along the belt between the rays of each of the pairs. The area in which the streamer belt intersects the ecliptic plane and which lies at the central meridian, will be recorded at the earth's orbit with a time delay of 5-6 days, in the form of one or several peaks with Nmax> 10cm-3. Furthermore, the simplest density profile of the portion of the HCS has the form of two peaks of a different or identical amplitude . The such a profile is observed in cases where the angle of intersection of the streamer belt with the ecliptic plane near the Sun is sufficiently large, i.e. close to 90°. The two-ray structure of the cross-section of the streamer-belt moves from the Sun to the Earth, it retains not only the angular size of the peaks but also the relative density variations, and the position of the neutral line (sector boundary) in between. At the Earth's orbit the ray structure of the streamer belt provides the source for sharp (i.e. with steep fronts of a duration of a few minutes or shorter) solar wind plasma density peaks (of a duration of several hours) with maximum values Nmax> 10cm-3.     

Space radiation environment in low earth orbit during influences from solar and geomagnetic events in December 2006

In low earth orbit, the SAA region is the dominant contributor to both proton environment and electron environment from the standpoint of radiation dose for spacecraft lifetime. However, the polar region and the horn region are sometimes strongly disturbed due to large solar and geomagnetic events. During large disturbances, enhancements in proton flux are measured in the polar region, which gives temporary more severe space radiation environment than that given in the SAA region. On the other hand, enhancements in electron flux are measured mainly in the horn region corresponding to the outer radiation belt, which are likely sources of high-energy electrons in the inner radiation belt. These short-term disturbances have another radiation hazard to spacecraft such as single event and electrostatic discharge.     

机器人修形磨削工具坐标系的精确标定方法

针对目前机器人修形磨削系统中接触轮姿态标定精度低影响磨削精度的问题,提出了一种实验测量的工具坐标系标定方法,姿态标定精度达0.05°.首先总结了通用静态标定法的不足之处,提出了新标定方法的构思并且理论证明了该方法的正确性.介绍了实验系统的组成,并在机器人砂带磨削系统上做了磨削实验.采集了磨削处的实验数据,分析实验数据,获得接触轮的实际偏转角,把偏转角补偿到磨削路径的工具坐标系上,最后完成了工具坐标系补偿后的重复性实验,证明了该方法的可行性和准确性.     

多自由度位移机构的设计

介绍了一套用于辅助计量测试的多自由度位移机构设计实例,讨论了各自由度的特点及不同实施方案.     

地效翼地面粘性效应风洞试验研究

为深入研究地面效应机理及地效翼空气动力特性,在同济大学上海地面交通工具风洞中心的空气动力-气动声学风洞内对地效翼模型进行了风洞试验。首先,根据地效翼空气动力特性及风洞试验能力,对风洞试验进行了设计;其次,在风洞试验中利用移动路面模拟系统和六分力天平测量系统,研究了地面粘性效应对地效翼空气动力的影响和地效翼空气动力特性。研究结果表明:固定地面附近边界层流动不仅与地效翼的高度有关,还与迎角有关;与移动地面相比,固定地面下测得的升力和阻力偏低,且由于固定地面边界层受气垫效应影响,失速延后。通过地效翼风洞试验研究揭示了移动路面模拟的重要性,并深入分析了地效翼空气动力特性,为地效飞行器空气动力设计和研究提供了参考。     

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.      

The response of African equatorial foF2 to geomagnetic storms: Comparison between observations and IRI-2007 predictions

This study examines the response of the African equatorial ionospheric foF2 to different levels of geomagnetic storms, using the foF2 hourly data for the year 1989 from Ouagadougou (12.4°N, 1.5°W, dip: 2.8°N). The study also compares the observed data for the selected storm periods with the latest IRI model (IRI-2007). The foF2 values (both observed and predicted) show typical features of daytime peak and post-midnight minimum peak. The response of the ionospheric foF2 over Ouagadougou to storms events, during the night-time and post-midnight hours indicates negative responses of the ionospheric foF2, while that of the daytime hours indicates positive responses. For the investigation on the variability of the observed foF2 with respect to IRI-2007 model, with the exception of the analysis of the 20–22, October, 1989 data, where a midday peak was also observed on the first day, this study reveals two characteristic daily foF2 variability peaks: post-midnight and evening peaks. In addition, for all the geomagnetic storms considered, the URSI and CCIR coefficients of the IRI-2007 model show reasonable correspondence with each other, except for some few discrepancies. For instance, the event of 28–30 August, 1989 shows comparatively higher variability for the URSI coefficient, and at the foF2 peak values, the event of 20–22 October, 1989 shows that the CCIR coefficient is more susceptible to foF2 variability than the URSI coefficient. This study is aimed at providing African inputs for the future improvement of the IRI model.     

A noise attenuation method for medium-energy electron measurements in the radiation belt

From the viewpoint of plasma particle measurements in the radiation belt, background noise is a serious problem. High-energy particles penetrating the sensor shielding generate spurious signals, and their count rate often can be comparable to the true signals. In order to attenuate such background noise during medium-energy (5–83 keV) electron measurements, we propose the double energy analyses (DEA) method. DEA is conducted by a combination of an electrostatic analyser (ESA) and avalanche photo-diodes (APDs); ESA and APD independently determine the energy of each incoming particle. By using the DEA method, therefore, the penetrating particles can be rejected when the two energy determinations are inconsistent; spurious noise are caused only when the deposited energy at an APD is by chance consistent with the measured energy by ESA. We formulate the noise count rate and show the advantage of DEA method quantitatively.