地球敏感器月球自主干扰保护异常分析及对策

针对某同步三轴稳定卫星地球敏感器自主干扰保护异常的问题,分析了地球敏感器受月球干扰的机理,详细比较了地面与星载月球干扰预报算法,挖掘比对了星载干扰保护软件数据,通过分析遥测数据及事后地面仿真计算软件处理验证,对异常点进行了准确定位,得出了星载月球干扰预报算法的局限性会导致卫星自主干扰保护异常的结论。并在此基础上,提出了在轨卫星地球敏感器受月球干扰自主保护异常时的处置对策,对后续同平台卫星相关设计提出了修改建议。     

蓄热式太阳能热光伏-热推进双模系统设计与性能分析

为有效解决在日蚀区太阳能热推进器推力失效、电力中断的问题,提出了蓄热式太阳能热光伏-热推进双模系统结构,并对系统各部件建立相关物理数学模型,分析了工质种类、工质流量等因素对推进性能的影响。结果表明,为保证推进器在日蚀区30min内持续提供推力和电力供应,砷化镓热光伏电池在无工质工况下能提供10W左右的低功率电力供应,在设计工况下能提供50W～110W的电力供应;液氢作为工质时,最大比冲将达到806s,随着工质流量的持续增加,比冲损失速率呈现先加快后减慢的变化趋势;液氨作为替代工质具有更快的加热速率,其比冲为240s～300s远低于氢工质比冲,其推力系数1.77要略高于氢工质推力系数1.7。通过本文研究,蓄热式太阳能双模推进系统具有较好的可行性,且推力及比冲适中,有望弥补低比冲化学推进和小推力电推进技术的不足。     

BME680压力传感器非线性补偿和温度补偿方法及实现

为了提高微机电系统(MEMS)压力传感器的测量精度,研究了压力传感器非线性补偿和温度补偿算法,提出了一种基于单片机的传感器非线性矫正方法,设计了一款集成数据采集系统、修正系统和传输系统的柔性压力片。采用一款商用MEMS压力传感器BME680进行了试验,利用Matlab软件对采集的数据进行分段多项式拟合,基于压力片MCU实现传感器误差的非线性补偿和实时修正。试验结果表明,温度补偿算法效果明显,压力传感器的静态输出精度提高明显,10℃及10℃以上,提高到0.207%FS;10℃以下,提高到1.39%FS,达到了预期要求。     

羊八井宇宙线强度观测数据的气压修正

分析了羊八井宇宙线强度的气压修正，分析表明，气压修正不仅与气压有关，而且与太阳活动有关．太阳活动最高的年，气压修正系数的绝对值最大．此外，计数率的修正值还与数据采样的时间间隔有关，即使是同一时间段，不同时间间隔采用率得到的修正值是不同的．本文最后分析了西藏羊八井中子监测器观测数据的气压修正，得到单路及八道多重计数的气压修正系数．     

太阳风质子束流密度的径向变化

利用Helios2飞船的数据,对太阳风速度分布中质子束流部分与整个质子的密度之比随日心距离的变化做了分析.为了排除碰撞因素的影响,有针对性地分析了太阳风高速流(600相似文献   

"神舟3号"运行高度上大气密度的变化

"神舟3号"(SZ-3)大气密度探测器搭载在SZ-3留轨舱上于2002年3月发射入轨,在轨运行期间获得了轨道舱运行高度范围(330-410km)内的大气密度数据.数据分析表明,无明显太阳和地磁扰动时,热层大气密度的主要变化之一是日照和阴影区域之间的涨落变化,最大涨落变化比约为3.0,变化比与太阳和地磁活动程度有关.在2002-04-17和2002-04-19的强地磁扰动时,全球热层大气密度上涨,同时在磁扰峰期探测获得30°N-40°N区域出现密度扰动异常现象.对强地磁扰动在运行轨道高度上大气密度最大涨幅约为60%左右,响应过程在时间上要比地磁扰动过程滞后6-7h,日照和阴影区域中大气密度的响应变化程度明显不同.在太阳活动程度发生变化时,热层大气密度会呈现出明显的正相关变化关系.     

天基X射线掠入射式成像望远镜发展现状

阐述了太阳X射线成像观测在空间天气预报中的地位和作用，叙述了掠入射式X射线聚焦成像的基本原理，简要介绍了在轨成功运行的天体X射线成像望远镜和太阳X射线成像望远镜的基本设计和技术指标，并介绍了国内正开发研制的专门服务于空间天气预报的太阳X射线成像望远镜基本设计和主要特点．     

High-cadence Hα imaging of solar flares

The Hα observation is a powerful tool to study the high-energy aspect of solar flares. Spiky brightenings of flare kernels at the Hα center reflect the rapid fluctuation in particle acceleration; linear polarization of Hα emission might be evidence of accelerated protons; red-shifts of the Hα line are caused by the chromospheric evaporation. To study the spiky brightenings of flare kernels with high-cadence imaging at the Hα center, a high-speed Hα camera for the Solar Flare Telescope at Mitaka, NAOJ, had been developed and it started the regular observation in 2001 July. However, the polarimetry and the Dopplermetry are also important and they are required to be carried out in parallel with the high-cadence imaging at the Hα center. Then, we upgraded the original high-speed Hα camera to a new Hα camera system for the multi-aspect Hα observations, which performs all of the high-cadence imaging, the linear polarization measurements, and the off-band imaging for velocity measurements. The new system started the observation in 2002 July. In this paper, the multi-aspect Hα imaging system is described and sample Hα images are presented.     

Energetic particle signatures of geoeffective coronal mass ejections

We have studied statistically associations of moderate and intense geomagnetic storms with coronal mass ejections (CMEs) and energetic particle events. The goal was to identify specific energetic particle signatures, which could be used to improve the predictions of the geoeffectiveness of full and partial halo CMEs. Protons in the range 1–110 MeV from the ERNE experiment onboard SOHO are used in the analysis. The study covers the time period from August 1996 to July 2000. We demonstrate the feasibility of energetic particle observations as an additional source of information in evaluating the geoeffectiveness of full and partial halo CMEs. Based on the observed onset times of solar energetic particle (SEP) events and energetic storm particle (ESP) events, we derive a proxy for the transit times of shocks driven by the interplanetary counterparts of coronal mass ejections from the Sun to the Earth. For a limited number of geomagnetic storms which can be associated to both SEP and ESP signatures, we found that this transit time correlates with the strength of geomagnetic storms.     

Solar wind velocity measurements near the sun using Ulysses radio amplitude correlations at two frequencies

Measurements of solar wind velocity have been derived from simultaneous coronal sounding observations of radio amplitude scintillations at both S-band and X-band during the solar conjunction of the Ulysses spacecraft in August 1991. The signal amplitude was recorded with an averaging time of 1 s. A cross-correlation analysis between S- and X-band amplitude fluctuations shows that the fluctuation signature at S-band appears to be shifted to earlier times with respect to the X-band recording. The time difference is proportional to the coronal separation of the ray paths and inversely proportional to the apparent velocity of plasma inhomogeneities across the ray paths. Preliminary estimates of solar wind speed obtained using model calculations of the differential refraction are found to lie near the expected transition from subsonic to supersonic velocities at solar offset distances of the order of 6–8 R. As a byproduct of the investigation, we find that the transition from weak to saturated scintillation occurs at about 16 R for S-band and 7 R for X-band.