Using high-energy proton fluence to improve risk prediction for consequences of solar particle events

The potential for exposure to large solar particle events (SPEs) with high energy levels is a major concern during interplanetary transfer and extra-vehicular activities (EVAs) on the lunar and Mars surface. Previously, we have used data from the last 5 solar cycles to estimate percentiles of dose to a typical blood-forming organ (BFO) for a hypothetical astronaut in a nominally shielded spacecraft during a 120-d lunar mission. As part of this process, we made use of complete energy spectra for 34 large historical SPEs to calculate what the BFO mGy-Eq dose would have been in the above lunar scenario for each SPE. From these calculated doses, we then developed a prediction model for BFO dose based solely on an assumed value of integrated fluence above 30 MeV (Φ₃₀) for an otherwise unspecified future SPE. In this study, we reasoned that since BFO dose is determined more by protons with higher energies than by those with lower energies, more accurate BFO dose prediction models could be developed using integrated fluence above 60 (Φ₆₀) and above 100 MeV (Φ₁₀₀) as predictors instead of Φ₃₀. However to calculate the unconditional probability of a BFO dose exceeding a pre-specified limit (“BFO dose risk”), one must also take into account the distribution of the predictor (Φ_30,Φ₆₀, or Φ₁₀₀), as estimated from historical SPEs. But Φ₆₀ and Φ₁₀₀ have more variability, and less available historical information on which to estimate their distributions over many SPE occurrences, than does Φ₃₀. Therefore, when estimating BFO dose risk there is a tradeoff between increased BFO dose prediction at a given energy threshold and decreased accuracy of models for describing the distribution of that threshold over future SPEs as the threshold increases. Even when taking the second of these two factors into account, we still arrived at the conclusion that overall prediction improves as the energy level threshold increases from 30 to 60 to 100 MeV. These results can be applied to the development of approaches to improve radiation protection of astronauts and the optimization of mission planning for future space missions.     

Induction of genomic instability after an acute whole-body exposure of mice to Fe ions

The purpose of this study was to evaluate dose–response relationships for the in vivo induction of micronuclei (MN) as a measure of both initial radiation damage and the induction of genomic instability. These measurements were made in mouse blood erythrocytes as a function of radiation dose, radiation quality, time after irradiation, and the genetic background of exposed individuals. Blood samples were collected from two strains of mouse (CBA/CaJ and C57BL/6J) at different times up to 3 months following a whole-body exposure to various doses of 1 GeV/amu ⁵⁶Fe ions (0, 0.1, 0.5 and 1.0 Gy, at the dose rate of a 1 Gy/min) or ¹³⁷Cs gamma rays (0, 0.5, 1.0 and 3.0 Gy, at the dose rate of 0.72 Gy/min). Blood-smear slides were stained with acridine orange (AO). The frequencies of MN were measured in mature normochromatic-erythrocytes (MN-NCEs) and in immature polychromatic-erythrocytes (MN-PCEs). Effects of both types of radiation on erythropoiesis were also evaluated. As a measure of cell progression delay, a dose-dependent decrease in numbers of PCEs was observed at day 2 post-exposure in both strains, regardless of radiation quality. Subsequently, the levels of PCEs increased in all exposed mice, reaching control levels (or higher) by day 7 post-exposure. Further, at day 2 after the exposure, there was no increase in the frequency of MN-PCEs in CBA/CaJ mice exposed to ⁵⁶Fe ions while the frequency of MN-PCEs elevated as a function of dose in the C57BL/6J mice. At day 4, there was no dose related increase in MN-NCEs in either strain of mouse exposed to ¹³⁷Cs gamma rays. Additionally, at the early sacrifice times (days 2 and 4), ⁵⁶Fe ions were slightly more effective (per unit dose) in inducing MN-NCEs than ¹³⁷Cs gamma rays in CBA/CaJ mice. However, there was no increase in the frequency of MN-NCEs at late times after an acute exposure to either type of radiation. In contrast, both types of radiation induced increased MN-PCEs frequencies in irradiated CBA/CaJ mice, but not C57BL/6J mice, at late times post-exposure. This finding indicates the potential induction of genomic instability in hematopoietic cells of CBA/CaJ mice by both types of radiation. The finding also demonstrates the influence of genetic background on radiation-induced genomic instability in vivo.     

影响PCL系统探测性能的因素分析

给出了可选作无源探测系统辐射源的信号参数,分析了目标的双基地等效反射面积、接收机噪声系数、干扰电平的组成及其相应的处理方法、PCL系统有效带宽和积累增益的关系,并对PCL系统的灵敏度和覆盖范围进行了研究.以此为基础,重新推导了双基地无源探测的距离方程.最后通过仿真分析了PCL系统可以获得的性能及其关键确定因素.     

Human response to high-background radiation environments on Earth and in space

The main long-term objective of the space exploration program is the colonization of the planets of the Solar System. The high cosmic radiation equivalent dose rate represents an inescapable problem for the safe establishment of permanent human settlements on these planets. The unshielded equivalent dose rate on Mars ranges between 100 and 200 mSv/year, depending on the Solar cycle and altitude, and can reach values as high as 360 mSv/year on the Moon. The average annual effective dose on Earth is about 3 mSv, nearly 85% of which comes from natural background radiation, reduced to less than 1 mSv if man-made sources and the internal exposure to Rn daughters are excluded. However, some areas on Earth display anomalously high levels of background radiation, as is the case with thorium-rich monazite bearing sand deposits where values 200–400 times higher than the world average can be found. About 2% of the world’s population live above 3 km and receive a disproportionate 10% of the annual effective collective dose due to cosmic radiation, with a net contribution to effective dose by the neutron component which is 3–4 fold that at sea level. Thus far, epidemiological studies have failed to show any adverse health effects in the populations living in these terrestrial high-background radiation areas (HBRA), which provide an unique opportunity to study the health implications of an environment that, as closely as possibly achievable on Earth, resembles the chronic exposure of future space colonists to higher-than-normal levels of ionizing radiation. Chromosomal aberrations in the peripheral blood lymphocytes from the HBRA residents have been measured in several studies because chromosomal damage represents an early biomarker of cancer risk. Similar cytogenetic studies have been recently performed in a cohort of astronauts involved in single or repeated space flights over many years. The cytogenetic findings in populations exposed to high dose-rate background radiation on Earth or in space will be discussed.     

Relation between galactic and solar cosmic radiation at aviation altitude

Cosmic radiation bombards us at high altitude with ionizing particles; the radiation has a galactic component, which is normally dominant, and a component of solar origin. Cosmic ray particles are the primary source of ionization in the atmosphere above 1 km; below 1 km radon is a dominant source of ionization in many areas.     

降落伞的计算机仿真研究

降落伞是一种应用广泛的气动力减速装置,其试验费用在整个开发、研制费用中,占有很大的比例。如何节省这笔费用,运用计算机仿真技术无疑是个最佳办法和途径。文章总结了降落伞仿真的一些情况和降落伞仿真所遇到的关键技术,并提出了在降落伞仿真中所面临的主要问题及解决这些问题的一般方法,可为降落伞研究提供参考。     

“实践五号”卫星星务管理系统

中国在“实践五号” (SJ- 5)卫星上首次应用并通过考验的星务管理系统 ,是实现卫星运行管理、自主控制、信息传送以及星地大回路操作的综合自动化系统。它是由计算机网络来协调、控制星上各种功能部件的相互联系 ,完成包括信息流、动作流、能量流的动态作业所形成的一种星载柔性服务系统。它具备有如下主要技术创新点 :构成整星多级控制 ;引入内嵌式管理执行单元 ;星上现场网络技术 ;构造硬件和软件的封装技术 ;利用商用实时多任务操作系统 ;兼容型分包遥测技术 ;复合型遥控和遥操作实现技术 ;信息多路径的冗余备份和系统重构技术 ;测试床技术 ;分级整体辐射加固技术。星务系统的应用既提高了整星自治能力 ,自动化和智能化水平 ,又分散了整星失误风险。从而 ,提高了整星级可靠性和运行功能的有效性。     

点阵结构部件的增材制造路径连接方法

旨在提高点阵结构部件增材制造的加工效率.点阵结构经分层切片后,每层将产生大量待填充多边形,通过将这些多边形抽象为离散点,并在切片层面内求解旅行商问题,进行连接路径的规划,进而获得高效率的点阵模型填充路径.算法综合考虑到旅行商问题的计算效率以及连接路径的计算总长:采用蚁群算法可获得无交叉连接轨迹,计算2000个点的连接规...     

高超声速钝锥模型及其尾迹红外辐射实验研究

介绍了利用InSb红外辐射计在弹道靶上测量底部直径为10mm、半锥角和头部半径分别为9°、2.2mm(模型A),8°、0.6mm(模型B)的两种非烧蚀钝锥模型及其尾迹的红外辐射.模型速度大于6km/s,飞行环境压力约4.8kPa,红外辐射测量波段为1~3μm、3~5μm.结果表明:非烧蚀钝锥模型头身部红外辐射远大于尾迹红外辐射,在相同飞行速度和环境压力条件下,模型A产生的红外辐射比模型B产生的红外辐射强.     

导弹蒙皮红外辐射特性的数值计算与分析

采用逆向蒙特卡罗(RMC)计算方法,在给定的飞行状态下分别计算出亚声速与超声速导弹蒙皮辐射源在不同方位角的2～μm、8～14 μm波段红外光谱辐射强度及强度场分布.结果表明:对亚声速导弹,相对于8～14 μm,其2～μm的辐射可忽略不计;对超声速导弹,相对于2～μm,其8～14 μm的辐射只有0%左右,但其绝对值较大而不可忽略不计.导弹的红外辐射在0°～90°探测位置内增加,在90°～180°内减小.大气对低空亚声速导弹辐射衰减作用强,对高空超声速导弹辐射衰减作用弱.超声速导弹的最大辐射强度是亚声速的18倍.