Relativistic electron fluxes and dose rate variations during April–May 2010 geomagnetic disturbances in the R3DR data on ISS

Space radiation has been monitored successfully using the Radiation Risks Radiometer-Dosimeter (R3D) installed at the ESA EXPOSE-R (R3DR) facility outside of the Russian Zvezda module of the International Space Station (ISS) between March 2009 and January 2011. R3DR is a Liulin type spectrometer–dosimeter with a single Si PIN detector 2 cm² of area and 0.3 mm thick. The R3DR instrument accumulated about 2 million measurements of the absorbed dose rate and flux of 10 s resolution. The total external and internal shielding before the detector of R3DR device is 0.41 g cm⁻². The calculated stopping energy of normally incident particles to the detector is 0.78 MeV for electrons and 15.8 MeV for protons. After the Coronal Mass Ejection (CME) at 09:54 UTC on 3 April 2010, a shock was observed at the ACE spacecraft at 0756 UTC on 5 April, which led to a sudden impulse on Earth at 08:26 UTC. Nevertheless, while the magnetic substorms on 5 and 6 of April were moderate; the second largest in history of GOES fluence of electrons with energy >2 MeV was measured. The R3DR data show a relatively small amount of relativistic electrons on 5 April. The maximum dose rate of 2323 μGy day⁻¹ was reached on 7 April; by 9 April, a dose of 6600 μGy was accumulated. By the end of the period on 7 May 2010 a total dose of 11,587 μGy was absorbed. Our data were compared with AE-8 MIN, CRESS and ESA-SEE1 models using SPENVIS and with similar observations on American, Japanese and Russian satellites.     

Modelling and observing Jovian electron propagation times in the inner heliosphere

The propagation of Jovian electrons in interplanetary space was modelled by solving the relevant transport equation numerically through the use of stochastic differential equations. This approach allows us to calculate, for the first time, the propagation time of Jovian electrons from the Jovian magnetosphere to Earth. Using observed quiet-time increases of electron intensities at Earth, we also derive values for this quantity. Comparing the modelled and observed propagation times we can gauge the magnitude of the transport parameters sufficiently to place a limit on the 6 MeV Jovian electron flux reaching Earth. We also investigate how the modelled propagation time, and corresponding Jovian electron flux, varies with the well-known ∼13 month periodicity in the magnetic connectivity of Earth and Jupiter. The results show that the Jovian electron intensity varies by a factor of ∼10 during this cycle of magnetic connectivity.     

PHITS simulations of the Protective curtain experiment onboard the Service module of ISS: Comparison with absorbed doses measured with TLDs

“Protective curtain” was the physical experiment onboard the International Space Station (ISS) aimed on radiation measurement of the dose – reducing effect of the additional shielding made of hygienic water-soaked wipes and towels placed on the wall in the crew cabin of the Service module Zvezda. The measurements were performed with 12 detector packages composed of thermoluminescent detectors (TLDs) and plastic nuclear track detectors (PNTDs) placed at the Protective curtain, so that they created pairs of shielded and unshielded detectors.     

太阳活动与全球气候变化

太阳不断向地球辐射电磁波和粒子, 太阳辐射是地球气候系统最主要的能量来源. 地球气候系统对太阳活动的响应是一个复杂的过程, 包括辐射过程、动力学过程以及微观物理过程等. 根据太阳辐射的卫星观测结果和重建结果, 例举了古气候、温度、大气环流和云量等方面太阳影响气候的观测证据, 论述了太阳影响气候的三种可能机制, 即太阳总辐射变化可以影响地表温度, 并通过海-气耦合改变大气环流; 太阳紫外辐射通过调制平流层的温度和风场影响下面的对流层; 太阳通过行星际磁场调制银河宇宙线, 而银河宇宙线通过电离大气影响云量, 进而改变地球的能量收支.      

厘米-分米波段Ⅲ型爆发的统计分析

统计分析了太阳第23周期间(2000年7月至2004年9月)在625~1500,MHz,2600~3800,MHz和5200~7600,MHz范围频谱仪观测到的Ⅲ型射电爆发. 给出了Ⅲ型爆发的分布、寿命、频率漂移率、偏振度和频率带宽. 结果显示, 频率漂移率和频率带宽的平均值随频率的增加而增大, 寿命和偏振度的平均值既不是常数也不是在宽频延伸上保持均匀不变的.最多的Ⅲ型爆发分布在625~3800,MHz范围内, 且随频率的增加而增多. 分析表明, 电子加速和能量释放地点主要是在分米波范围内, 这个频率范围的特征可能与分米波段上的磁位形有关, 并且与主耀斑地点附近磁重联区中的电子加速有关. 然而, 还有相当数量的Ⅲ型爆发发生在5200~7600,MHz范围内, 这个特征表明电子加速的地点是在一个日冕的宽范围中. 关于厘米relax-relax 分米波段Ⅲ型爆发的辐射机制最可能包含相干的等离子体辐射或电子回旋脉泽辐射过程.      

飞机进近着陆电磁环境建模与辐射分布分析

机场终端区电磁、地形和地物在拓扑、物理和语义上的异构性导致进近着陆电磁环境构成机理复杂,很难用单尺度解析模型表征电磁环境的本质属性.在分析终端区多要素层次构成机理和关联耦合特征的基础上,提出一种多层融合的进近着陆电磁环境模型架构.综合采用矩量法和射线追踪法模拟台站辐射特性和地空电波传播模式,建立进近着陆区域电磁辐射强度量化表征与空间分布计算模型,有效降低了场边界特性不规则时空变化带来的电波预测误差.结合某机场地形和航向台数据,对终端区主航道和余隙航道的电磁辐射强度和覆盖范围进行计算和对比分析.仿真结果验证了本建模与分析方法的有效性.     

飞行弹丸红外特性的地面模拟试验

设计并建立了用于飞行弹丸中段飞行状态实验室模拟的试验系统,测量获得了飞行弹丸的红外辐射特性.基于传热与辐射理论,分析了相关参数对实验结果的影响,获得飞行弹丸在一定飞行状态下的辐射特性变化规律.目标的初始温度和辐照条件是影响目标辐射特性的主要因素,自旋状态影响辐射特性的空间分布.试验测量与数值仿真和理论分析结果均具有很好的一致性,证明在实验室开展飞行弹丸的红外辐射特性模拟试验具有可行性.     

电离辐照诱发面阵电荷耦合器暗信号增大试验

针对电荷耦合器件(CCD)在空间轨道环境中应用时易受到辐射损伤的影响,对面阵CCD的电离辐照损伤效应问题进行了试验研究.首先,通过开展面阵CCD60 Co γ射线电离辐照效应试验,在暗场条件下测试了面阵CCD辐照后输出信号随积分时间的变化,并拟合计算出暗信号斜率.然后,对比分析了不同偏置条件下辐照后暗信号退化的试验规律;分析了不同偏置条件下辐照后暗信号的退火恢复情况;分析了不同积分时间、不同总剂量下的暗信号不均匀性的变化规律.最后,阐述了电离辐照损伤诱发面阵CCD暗信号增大的物理机制.结果表明:面阵CCD对电离辐照损伤很敏感,在进行航天器成像系统设计时,要充分考虑CCD受电离辐照损伤带来的影响.     

我国空间电力线谐波辐射现象分析

研究了利用DEMETER卫星电磁场探测数据辨识电力线谐波辐射(PLHR,Power Line Harmonic Radiation)事件的方法,探讨了我国空间中PLHR事件的特点.通过采用时频分析和Welch功率谱估计法分析了2005-2010年6年我国空间中的全部卫星电场强度探测数据,共发现151例PLHR事件,给出了PLHR事件的统计分析和典型实例.结果表明我国空间PLHR事件的频率分布在1 000~4 500 Hz之间,多为50 Hz的奇数倍,间隔为50/100 Hz.PLHR事件与我国电网发展和变化有密切关系,与地磁活动水平无关,呈现出昼夜差异和季节差异.最后给出了影响PLHR事件探测的可能因素.     

Method for the prediction of the effective dose equivalent to the crew of the International Space Station

This paper describes a methodology for assessing the pre-mission exposure of space crew aboard the International Space Station (ISS) in terms of an effective dose equivalent. In this approach, the PHITS Monte Carlo code was used to assess the particle transport of galactic cosmic radiation (GCR) and trapped radiation for solar maximum and minimum conditions through an aluminum shield thickness. From these predicted spectra, and using fluence-to-dose conversion factors, a scaling ratio of the effective dose equivalent rate to the ICRU ambient dose equivalent rate at a 10 mm depth was determined. Only contributions from secondary neutrons, protons, and alpha particles were considered in this analysis.