Spectroscopic Measurement of Coronal Compositions

Although the elemental composition in all parts of the solar photosphere appears to be the same this is clearly not the case with the solar upper atmosphere (SUA). Spectroscopic studies show that in the corona elemental composition along solar equatorial regions is usually different from polar regions; composition in quiet Sun regions is often different from coronal hole and active region compositions and the transition region composition is frequently different from the coronal composition along the same line of sight. In the following two issues are discussed. The first involves abundance ratios between the high-FIP O and Ne and the low-FIP Mg and Fe that are important for meaningful comparisons between photospheric and SUA compositions and the second involves a review of composition and time variability of SUA plasmas at heights of 1.0≤h≤1.5R _⊙.     

The Genesis Solar Wind Concentrator Target: Mass Fractionation Characterised by Neon Isotopes

The concentrator on Genesis provided samples of increased fluences of solar wind ions for precise determination of the oxygen isotopic composition. The concentration process caused mass fractionation as a function of the radial target position. This fractionation was measured using Ne released by UV laser ablation and compared with modelled Ne data, obtained from ion-trajectory simulations. Measured data show that the concentrator performed as expected and indicate a radially symmetric concentration process. Measured concentration factors are up to ∼30 at the target centre. The total range of isotopic fractionation along the target radius is 3.8%/amu, with monotonically decreasing ²⁰Ne/²²Ne towards the centre, which differs from model predictions. We discuss potential reasons and propose future attempts to overcome these disagreements.     

Sharp boundaries of solar wind plasma structures and their relationship to solar wind turbulence

Sharp (<10 min) and large (>20%) solar wind ion flux changes are common phenomena in turbulent solar wind plasma. These changes are the boundaries of small- and middle-scale solar wind plasma structures which can have a significant influence on Earth’s magnetosphere. These solar wind ion flux changes are typically accompanied by only a small change in the bulk solar wind velocity, hence, the flux changes are driven mainly by plasma density variations. We show that these events occur more frequently in high-density solar wind. A characteristic of solar wind turbulence, intermittency, is determined for time periods with and without these flux changes. The probability distribution functions (PDF) of solar wind ion flux variations for different time scales are calculated for each of these periods and compared. For large time scales, the PDFs are Gaussian for both data sets. For small time scales, the PDFs from both data set are more flat than Gaussian, but the degree of flatness is much larger for the data near the sharp flux change boundaries.     

What Determines the Composition of SEPs in Gradual Events?

Gradual solar energetic particle (SEP) events are evidently accelerated by coronal/interplanetary shocks driven by coronal mass ejections. This talk addresses the different factors which determine the composition of the accelerated ions. The first factor is the set of available seed populations including the solar wind core and suprathermal tail, remnant impulsive events from preceding solar flares, and remnant gradual events. The second factor is the fractionation of the seed ions by the injection process, that is, what fraction of the ions are extracted by the shock to participate in diffusive shock acceleration. Injection is a controversial topic since it depends on the detailed electromagnetic structure of the shock transition and the transport of ions in these structured fields, both of which are not well understood or determined theoretically. The third factor is fractionation during the acceleration process, due to the dependence of ion transport in the turbulent electromagnetic fields adjacent to the shock on the mass/charge ratio. Of crucial importance in the last two factors is the magnetic obliquity of the shock. The form of the proton-excited hydromagnetic wave spectrum is also important. Finally, more subtle effects on ion composition arise from the superposition of ion contributions over the time history of the shock along the observer’s magnetic flux tube, and the sequence of flux tubes sampled by the observer.     

强辐射条件下应变测量的抗干扰技术研究

文章从动力学结构分析应变测量的基本原理入手,着重介绍了国防高科技试验中,在强辐射、强电磁脉冲干扰环境条件下,为保证应变测量的实现,经模拟试验研究,在应变测量时采用了一系列抗干扰技术措施,包括特殊环境条件下所用元器件材料的选择,传感应变计安装方式,组桥接线方式,密封屏蔽等技术。并介绍了这些技术措施在某试验现场应变测试试验中的应用概况.     

Relationship between daily variation of cosmogenic nuclide Be-7 concentration in atmosphere and solar activities

Daily Be-7 concentrations in air at the height of 15 m are continuously observed at 38°15.2′N, 140°20.9′E, between 2000 and 2001. The average concentration and the relative standard deviation were 4.0 mBq/m³ and 50% in 2000–2001, respectively. The Be-7 concentrations increased 2.5% with the decrease in the sunspot numbers by 6.7% for the term of two years. From the power spectral analysis, the periodicity of 26 days is shown for the daily Be-7 concentrations. The folding analysis indicates that the time variation of the Be-7 concentration is similar to that of the ground-based neutron counting rate, and the phase delay for the minimum portion of Be-7 concentration was roughly 8 days to the maximum sunspot number. These results indicate that the Be-7 concentrations in the air at ground level have 26 day periodicity as a component of time variations and the time variation is caused by the solar modulation of galactic cosmic rays, which corresponds to the variation of the sunspot number due to the rotation of the sun.     

基于蒙特卡罗法辐射传递系数的统计分析

文章基于蒙特卡罗方法定义了表面热辐射换热辐射传递系数的表达式,确定其概率分布和置信度水平并进行统计分析。推导封闭腔内辐射传递系数的相对和绝对误差公式,为求解辐射传递系数所需追踪射线数量提供参考依据。     

空间实验室大面积太阳电池阵技术研究

介绍了空间实验室大面积太阳电池阵的方案构型，并进行了模态分析、热结构耦合分析和动力学仿真分析。生产出了全尺寸的集成演示样机，进行了展开试验、主展开机构的模态试验，以及半刚性太阳电池板和二自由度驱动机构的振动试验。计算和试验结果表明，技术方案是可行的。     

弹道靶红外辐射测量

为深入认识再入物理现象 ,在弹道靶上做了模型头部和近尾流红外辐射测量。发射器为 1 4.5mm口径的二级轻气炮 ,模型为1 0mm的球 ,材料为聚碳酸酯和铝 ,模型发射速度 4～6km/s,使用红外InSb探测器测量波长 3～ 5 .4μm的红外辐射 ,靶室压力 5 .32kPa。实验中使用光电法测量模型速度 ,两站阴影照相进行模型姿态监测和速度核实。实验结果表明 :球模型的红外辐射强度强烈依赖于模型材料和模型飞行速度。对不同材料模型头部和尾流部辐射强度的定性比较说明由于低温材料烧蚀产物的存在 ,极大地增强了头部和近尾流区的辐射强度 ,而且延长了尾流辐射长度     

动态差压检测系统的共模误差研究

主要针对以差压变送器为核心的动态差压检测系统的特点 ,应用流体网络分析方法 ,提出了动态差压检测系统中的共模误差问题。理论分析和仿真计算结果表明 :共模误差与检测系统两侧引压管路的不一致性直接相关 ,为了获得动态差压信号的准确检测 ,必须对动态差压检测系统的共模误差予以抑制