无人值守型手部α和β污染监测仪的研制

介绍了一种新型的无人值守型手部α,β污染监测仪,该仪器易于携带和安装,能够自动同时进行α,β污染监测,结构设计上避免了监测中的二次污染问题。 对防止核污染扩散及现场工作人员的安全有着十分重要的意义。     

The extension of the INCL model for simulation of shielding in space

Radiation hazard for space missions is mainly due to cosmic ray protons, helium nuclei and light ions, whose energy spectrum is maximum around 1 GeV per nucleon but remains non-negligible for energies up to 15 GeV per nucleon. Nuclear reactions induced by high energy protons are often described by intranuclear cascade plus evaporation models. The attention is focused here on the Liège Intranuclear Cascade model (INCL), which has been shown to reproduce fairly well a great deal of experimental data for nucleon-induced reactions in the 200 MeV to 2 GeV range, when coupled with the ABLA evaporation-fission code. In order to extend the model to other conditions relevant for space radiation, three improvements of INCL are under development. They are reported on here. First, the reaction model has been extended to nucleon–nucleus reactions at incident energies up to 15 GeV, mainly by the inclusion of additional pion production channels in nucleon–nucleon collisions during the cascade. Second, a coalescence mechanism for the emission of light charged particles has been implemented recently. Finally, the model has been modified in order to accommodate light ions as projectiles. First results are shown and compared with illustrative experimental data. Implications for issues concerning radiation protection in space are discussed.     

基于ELMo-GCN的核电领域命名实体识别

在核电领域的知识管理过程中,需要使用命名实体识别技术抽取高质量语义实体,以进行核电领域文本的智能分析和处理。在现有研究的基础上,通过增强网络对上下文信息的提取能力,提升模型对嵌套命名实体的识别准确率。经实验验证,所提方法较现有方法在准确率与召回率指标上提升显著,与BiFlaG网络对比,准确率提高9.52%,召回率提高8.51%,F₁值提高9.02%。所提方法对嵌套命名实体识别优于BiFlaG等网络。     

Measurement of cosmic ray elemental composition from the CAKE balloon experiment

CAKE (Cosmic Abundances below Knee Energies) was a prototype balloon experiment for the determination of the charge spectra and abundances of the primary cosmic rays (CR) with Z > 10. It was a passive instrument made of layers of CR39® and Lexan®/Makrofol® nuclear track detectors; it had a geometric acceptance of ∼0.7 m² sr for Fe nuclei. Here, the scanning and analysis strategies, the algorithms used for the off-line filtering and for the tracking in automated mode of the primary cosmic rays are presented, together with the resulting CR charge distribution and their abundances.     

核电站工作场所中子能谱和周围剂量当量率测量

中子周围剂量当量是核电站辐射防护监测的主要对象之一,而中子周围剂量当量的评估强烈依赖中子的能量分布。利用自制的多球谱仪对秦山第三核电有限公司（TQNPC）重水反应堆安全壳内5个位置的中子能谱和周围剂量当量率进行了测量。该谱仪由1个³He正比计数器以及9个2.5～12英寸不同直径的聚乙烯球组成,响应函数通过MCNP程序计算,并利用标准²⁵²Cf中子源进行了校准和验证。通过测量的中子能谱,获得了不同工作区域的中子周围剂量当量率及其能量分布,并与中子周围剂量当量率仪和CR-39径迹蚀刻探测器的测量结果进行了比较,为核电站中子剂量的监测提供了相关参考数据。     

Extension of INCL4 between 2 and 15 GeV

The intranuclear cascade model INCL4 has been shown to be very successful for describing, without adjustable parameters, a whole set of data for p-induced reactions in the 40 MeV–2 GeV energy range. In view of its possible application to cosmic ray interactions, the INCL4 code has been extended to the 2–15 GeV energy range, so covering a large part of the spectrum of the incident energy of the cosmic rays.     

空间核动力源的安全性研究进展

同位素热/电源以及空间核反应堆在深空探测任务中有重要应用。通过调研其技术特点以及国际上针对核能空间应用安全性的相关规范,研究了其空间安全性规范的法律法规。以ALRH(Apollo Lunar Radiosotope Heater,阿波罗月球任务同位素热源)、GPHS(General Purpose Heater Source,通用型热源)、LWRHU(Lighted Weighted Radiosotope Heater Unit,轻量放射性同位素热源)、MMRTG(Multi-Mission Radioisotope Thermoelectric Generator,多任务型放射性同位素电源)等同位素热/电源及俄罗斯热离子空间反应堆电源(TOPAZ-II型号)为例,结合美俄开展的同位素热/电源的系列安全性试验,重点关注了不同型号的试验及分析技术细节,并分析了同位素热/电源的空间应用安全评价方法,可为开展相关研发提供技术参考。     

Assessment and requirements of nuclear reaction databases for GCR transport in the atmosphere and structures

The transport properties of galactic cosmic rays (GCR) in the atmosphere, material structures, and human body (self-shielding) are of interest in risk assessment for supersonic and subsonic aircraft and for space travel in low-Earth orbit and on interplanetary missions. Nuclear reactions, such as knockout and fragmentation, present large modifications of particle type and energies of the galactic cosmic rays in penetrating materials. We make an assessment of the current nuclear reaction models and improvements in these model for developing required transport code data bases. A new fragmentation data base (QMSFRG) based on microscopic models is compared to the NUCFRG2 model and implications for shield assessment made using the HZETRN radiation transport code. For deep penetration problems, the build-up of light particles, such as nucleons, light clusters and mesons from nuclear reactions in conjunction with the absorption of the heavy ions, leads to the dominance of the charge Z = 0, 1, and 2 hadrons in the exposures at large penetration depths. Light particles are produced through nuclear or cluster knockout and in evaporation events with characteristically distinct spectra which play unique roles in the build-up of secondary radiation's in shielding. We describe models of light particle production in nucleon and heavy ion induced reactions and make an assessment of the importance of light particle multiplicity and spectral parameters in these exposures.     

电化学过程中的局域核反应及动态Casimir效应

通过CR-39固体径迹探测器、钯阴极的辐射自照相等方法观察到了电解过程中的局域核反应.综合国内外相关研究数据,认为电解过程中,电极尖端处出现的动态Casimir效应,及涡漩运动与零点能相干效应而提取真空能,是电化学异常放热的来源,少量具有滞后和积累效应的、高度定向的极化核反应,可以用具有轴向高能宇宙射线的类星体涡旋模型加以解释.讨论了真空零点电磁涨落和挠场理论,及有关实验现象.利用推出的类星体涡旋模型理论,可以对自然界和实验室中出现的许多异常现象进行解释.      

Sources of inner radiation zone energetic helium ions: Cross-field transport versus in-situ nuclear reactions

Radial transport theory for inner radiation zone MeV He ions has been extended by combining radial diffusive transport, losses due to Coulomb friction and charge exchange reaction with local generation of ³He and ⁴He ions due to nuclear reactions taking place on the inner edge of the inner radiation zone. From interactions between high energy trapped protons and upper atmospheric constituents we have included a nuclear reaction yield helium flux source that was numerically derived from a nuclear reaction model originally developed at the Institute of Nuclear Researches of Moscow, Russia and implemented in the computer system at the University of Campinas, Brazil. Magnetospheric transport computations have been made covering the L-shell range L=1.0 to 1.6 and the resulting MeV He ion flux distributions show a strong influence of the local nuclear source mechanism on the inner zone energetic He ion content.     

Hot atoms in cosmic chemistry

High energy chemical reactions and atom molecule interactions might be important for cosmic chemistry with respect to the accelerated species in solar wind, cosmic rays, colliding gas and dust clouds and secondary knock-on particles in solids. “Hot” atoms with energies ranging from a few eV to some MeV can be generated via nuclear reactions and consequent recoil processes. The chemical fate of the radioactive atoms can be followed by radiochemical methods (radio GC or HPLC). Hot atom chemistry may serve for laboratory simulation of the reactions of energetic species with gaseous or solid interstellar matter. Due to the effective measurement of 10⁸–10¹⁰ atoms only it covers a low to medium dose regime and may add to the studies of ion implantation which due to the optical methods applied are necessarily in the high dose regime.

Experimental results are given for the systems: C/H₂O (gas), C/H₂O (solid, 77 K), N/CH₄ (solid, 77K) and C/NH₃ (solid, 77 K). Nuclear reactions used for the generation of 2 to 3 MeV atoms are: ¹⁴N(p, ) ¹¹C, ¹⁶O(p, pn) ¹¹C and ¹²C(d,n) ¹³N with 8 to 45 MeV protons or deuterons from a cyclotron. Typical reactions products are: CO, CO₂, CH₄, CH₂O, CH₃OH, HCOOH, NH₃, CH₃NH₂, cyanamide, formamidine, guanidine etc. Products of hot reactions in solids are more complex than in corresponding gaseous systems, which underlines the importance of solid state reactions for the build-up of precursors for biomolecules in space. As one of the major mechanisms for product formation, the simultaneous or fast consecutive reactions of a hot carbon with two target molecules (reaction complex) is discussed.     

临近空间大气中子诱发电子器件单粒子翻转模拟研究

根据重离子试验数据, 采用长方体(RPP)模型, 用GEANT4软件工具包编程, 建立了垂直于器件表面入射的中子诱发电子器件的单粒子翻转模型. 考虑敏感体积及其附近的次级粒子对单粒子翻转的贡献, 统计了次级粒子在敏感体积内沉积能量的微分能谱分布, 对在敏感体积内沉积不同能量的次级粒子对单粒子翻转的贡献进行了区分计算, 模拟计算结果与地面试验结果符合较好.      

Trapped antiprotons produced by cosmic rays in the Earth's magnetosphere.

The existence of significant fluxes of antiparticles in the Earth magnetosphere has been predicted on theoretical considerations in this article. These antiparticles (positrons or antiprotons) at several hundred kilometers of altitudes, we believe are not of direct extraterrestrial origin, but are the natural products of nuclear reactions of the high energy primary cosmic rays (CR) and trapped protons (TP) confined in the terrestrial radiation belt, with the constituents of terrestrial atmosphere. Extraterrestrial positrons and antiprotons born in nuclear reactions of the same CR particles passing through only 5-7 g/cm2 of interstellar matter, exhibit lower fluxes compared to the antiprotons born at hundreds of g/cm2 in the atmosphere, which when confined in the magnetic field of the Earth (in any other planet), get accumulated. We present the results of the computations of the antiproton fluxes at 10 MeV to several GeV energies due to CR particle interactions with the matter in the interstellar space, and also with the residual atmosphere at altitudes of approximately 1000 km over the Earth's surface. The estimates show that the magnetospheric antiproton fluxes are greater by two orders of magnitude compared to the extraterrestrial fluxes measured at energies <1-2 GeV.     

Ground-based measurements of galactic cosmic ray fragmentation in shielding.

The mean free path for nuclear interactions of galactic cosmic-rays is comparable to shielding and tissue thicknesses present in human interplanetary exploration, resulting in a significant fraction of nuclear reaction products at depth. In order to characterize the radiation field, the energy spectrum, the angular distribution, and the multiplicity of each type of secondary particles must also be known as a function of depth. Reactions can take place anywhere in a thick absorber; therefore, it is necessary to know these quantities as a function of particle energy for all particles produced. HZE transport methods are used to predict the radiation field; they are dependent on models of the interaction of man-made systems with the space environment to an even greater extent than methods used for other types of radiation. Hence, there is a major need to validate these transport codes by comparison with experimental data. The most cost-effective method of validation is a comparison with ground-based experimental measurements. A research program to provide such validation measurements using neon, iron and other accelerated heavy ion beams will be discussed and illustrated using results from ongoing experiments and their comparison with current transport codes. The extent to which physical measurements yield radiobiological predictions will be discussed.     

水下燃料组件转运系统耦合振动分析

核动力厂燃料组件转运系统运行的平稳性和系统结构的可靠性对确保燃料组件安全至关重要。为了解运行过程中系统的振动情况，建立了考虑水影响的梁-小车+刚性杆-质量+弹簧+阻尼的耦合系统动力学模型，推导了系统的非线性运动微分方程。在此基础上，采用数值算法计算了小车在不同行走速度下系统的响应。研究结果表明:运行过程中，小车行走速度越小系统振动越弱，相对越平稳；由于静变形，即使小车行走速度很低，吊篮仍会承受一定的横向力作用，需注意吊篮薄弱部位的强度；导轨支撑附近位置为吊篮的相对危险位置，必要时可以在此设置监测点以保证燃料组件安全。      

An improved Green's function for ion beam transport.

Ion beam transport theory allows testing of material transmission properties in the laboratory environment generated by particle accelerators. This is a necessary step in materials development and evaluation for space use. The approximations used in solving the Boltzmann transport equation for the space setting are often not sufficient for laboratory work and those issues are the main emphasis of the present work. In consequence, an analytic solution of the linear Boltzmann equation is pursued in the form of a Green's function allowing flexibility in application to a broad range of boundary value problems. It has been established that simple solutions can be found for high charge and energy (HZE) ions by ignoring nuclear energy downshifts and dispersion. Such solutions were found to be supported by experimental evidence with HZE ion beams when multiple scattering was added. Lacking from the prior solutions were range and energy straggling and energy downshift with dispersion associated with nuclear events. Recently, we have found global solutions including these effects providing a broader class of HZE ion solutions.     

Long-term space flights--personal impressions.

During a final 4-month stage of a 1-year space flight of cosmonauts Titov and Manarov, a physician, Valery Polyakov was included on a crew for the purpose of evaluating their health, correcting physical status to prepare for the spacecraft reentry and landing operations. The complex program of scientific investigations and experiments performed by the physician included an evaluation of adaptation reactions of the human body at different stages of space mission using clinicophysiological and biochemical methods; testing of alternative regimes of exercise and new countermeasures to prevent an unfavourable effect of long-term weightlessness.     

Hydrodynamical evolution of AGN driven by radiation from circumnuclear starbursts

We explore the hydrodynamical evolution of dusty gas around active galactic nuclei (AGN) driven by the radiation from circumnuclear starbursts. For this purpose, we calculate the temporal equilibrium states between the radiation force by starburst regions and the gravity in galactic nuclei. As a result, we find that the equilibrium patterns between the radiation force and the gravity are roughly characterized by three types. The first is the situation where the starburst luminosity is larger than the Eddington luminosity. In this case, the dusty gas is blown out like a wind. We may detect intense infrared (IR) radiation from the starburst regions screened by blown-out dusty gas. The second is the situation when the radiation force is comparable to the gravity. In this case, the equilibrium surface surrounds the nuclear regions as well as starburst regions. Since the dusty gas absorbs UV or soft X-rays from the center and re-emits IR radiation, we may recognize it as a Seyfert 2 galaxy. The last is the situation where the starburst luminosity is small. In this case, the dusty wall of equilibrium would be built up only in the vicinity of starburst regions. The radiation from central regions is rarely obscured, because the dusty regions have only small angular extension. So, it would look like a Seyfert 1 galaxy which is characterized by intense soft X-rays. When we consider the stellar evolution in starburst regions, the starburst luminosity decreases with time. Therefore, we can recognize the above three types as time evolution; a starburst galaxy (first stage), a Seyfert 2 galaxy (second stage), and a Seyfert 1 galaxy (third stage). Note that we present here an alternative scenario for explaining the relation between Sy 1's and Sy 2's to the standard “Unified Scheme”.