高分辨椭圆弯晶谱仪在激光等离子体实验中的应用

 描述了用于激光等离子体X射线光谱研究的椭圆弯曲晶体谱仪系统。在“神光Ⅱ”第九路激光上对该谱仪进行标定实验，利用CCD相机成功地获得了激光等离子体铝和钛离子的K壳层和金离子M壳层谱；通过研究和辨认谱线，得到了X射线光谱，同时还给出了实验测定的谱仪分辨率。椭圆弯曲晶体谱仪除有高的收集光子效率外，还有更好的谱分辨和空间分辨率。分析了椭圆弯曲晶体谱仪在前沿科学技术和高技术实验中的应用。     

EAST高时空分辨极向弯晶谱仪系统的升级及初步实验结果

为了拓宽等离子体参数测量范围,对EAST极向弯晶谱仪(PXCS)进行了升级改造。配合高通量大面积水冷固体探测器,提高了极向弯晶谱仪系统的光子计数率、时间分辨率、空间探测范围以及长时间运行稳定性,并在EAST装置上成功运行。实验结果表明,升级后的谱仪获得了高信噪比的类氦氩离子的母线及其一系列伴线谱,通过光谱拟合分析给出了等离子体温度时间演化及其剖面信息,测量结果与切向弯晶谱仪的数据一致,验证了极向弯晶谱仪的升级结果和数据测量的可靠性,并且在EAST长脉冲实验运行也能够稳定地提供全时间的参数分布。     

EAST高时空分辨极向弯晶谱仪系统的升级及初步实验结果

为了拓宽等离子体参数测量范围,对EAST极向弯晶谱仪(PXCS)进行了升级改造。配合高通量大面积水冷固体探测器,提高了极向弯晶谱仪系统的光子计数率、时间分辨率、空间探测范围以及长时间运行稳定性,并在EAST装置上成功运行。实验结果表明,升级后的谱仪获得了高信噪比的类氦氩离子的母线及其一系列伴线谱,通过光谱拟合分析给出了等离子体温度时间演化及其剖面信息,测量结果与切向弯晶谱仪的数据一致,验证了极向弯晶谱仪的升级结果和数据测量的可靠性,并且在EAST长脉冲实验运行也能够稳定地提供全时间的参数分布。     

软X射线晶体谱仪

描述了用于激光等离子体软Ｘ射线光谱学研究长波晶体谱仪。用具有大晶格常数的晶体，极薄的滤片和对软Ｘ射线灵敏的底片，获得了波长达５．８ｎｍ的激光等离子体软件Ｘ射线光谱。同时还给出了实验测定了谱仪光谱分辨率。     

平场光栅谱仪相对衍射效率测量

 以激光碳等离子体作为软X射线源,同时用平场光栅谱仪、常栅距光栅谱仪测量了类氢和类氦离子谱线强度,以一级谱线强度为标准,给出了平场光栅谱仪高级次光谱的相对衍射效率。     

圆柱面和圆锥面弯晶谱仪的理论计算及设计

用光线追迹的方法对圆柱面和圆锥面弯晶谱仪进行了理论计算,得到了谱仪的空间与色散坐标、线色散率、角色散率、光谱分辨力、空间和光谱放大率以及谱仪亮度等参数的解析计算公式,并对两类谱仪进行了具体的参数设计及性能比较.结果表明,圆锥面弯晶谱仪比同类型的传统圆柱面弯晶谱仪有着更为良好的聚焦性能,能够进一步改善谱仪的光子收集效率、谱仪亮度以及空间分辨力.这项工作为谱仪研制提供了理论基础和设计依据.     

一台入射距离为155mm的XUV平场光谱仪

利用光路追踪程序对不同入射距离的变栅距平场光栅的成像进行了研究和设计。在此基础上研制了一台与传统平场光栅谱仪不同的入射狭逢到光栅中心距离为 1 55mm的掠入射平焦场谱仪。该谱仪的波段范围为 4～ 4 0 nm,光谱分辨率为 0 .0 1 nm。利用该谱仪成功地获得了 Ti元素的激光等离子体光谱。     

钴、镍和铜离子的类钠件线谱

以激光辐照固体平面靶产生的高温等离子体作为辐射源,利用平晶x射线谱仪观测了钴、镍和铜的类氖离子2p-3d跃迁的长波类钠伴线x射线光谱。根据等电子数序规律外推,与观测波长值比较,给出了对这些伴线进行辨认的结果。     

北京谱仪(BESⅡ)的飞行计数器(TOF)时间和分辨率的修正

随着北京谱仪上5800万J/ψ数据的获取,为了获得较好的物理结果,必须有很好的粒子鉴别.鉴于北京谱仪Ⅱ飞行时间计数器(TOF)对粒子鉴别的特殊重要性,有必要对飞行时间计数器的时间测量和分辨率进行研究.本文利用北京谱仪Ⅱ已获取的5800万J/ψ数据,对飞行时间计数器的时间和分辨率进行修正,最后给出修正结果以及修正后的鉴别效率.     

激光拉曼光谱仪的全系统校正

提出了一套对激光拉曼光谱仪进行全系统校正的完整方案，并在一台ＳＰＥＸ １４３０型双单色仪单道拉曼光谱仪上全面实现了这套校正，包括谱仪的波数精度及重现性，狭缝函数，光谱分辨率，功率传递系数，光谱响应，偏振光谱响应，偏振传递性能及寄生谱带检查。结果表明，在激光拉曼谱测量中许多源于光谱仪体系的测量误差实际上是不可避免的，因此对常用的谱仪要作日常的状态监控和至少一次全面系统校正，是激光拉曼谱学研究的先决条     

核材料γ能谱指纹模糊识别机理研究

以γ射线的能量与强度所构成的二维平面为论域,提出了关于γ射线能谱的二维模糊集合的概念,建立了γ射线能谱二维模糊集合隶属函数.提出和介绍了γ射线能谱指纹模糊识别的基本原理与方法.通过对γ能谱数据的归一化处理,实现了γ射线能谱指纹的类型识别和个体识别.通过引入识别增强因子,获得了较高的识别置信度.对模拟放射性物质的γ射线能谱指纹进行了识别研究,探讨了系统统计涨落以及探测距离变化对识别隶属度的影响.研究表明,γ射线能谱指纹模糊识别方法具有较强的类型识别能力和个体识别能力,可应用于核安全保障等领域. 关键词： γ能谱指纹 模糊识别 核材料     

基于模糊识别的γ能谱定性分析

提出了一种基于模糊识别的γ能谱分析方法。通过建立关于未知谱的模糊集合、标准核素库及模糊识别算法,实现了γ能谱的快速自动定性分析,并对3组混合标准源γ能谱和3个低本底样品γ能谱进行了定性分析。结果表明在不精确求解峰位的情况下,即可准确分析出样品中所含的放射性核素。     

Gamma holography from multiple scattering

Since the introduction of heterodyne methods for synchrotron radiation (Cousesement et al. in Phys. Rev. B 54:16003, 1996; Callens et al. in Phys. Rev. 67:104423, 2003) one observes interferences between two scattering amplitudes; the scattering amplitude of resonant nuclei in a reference sample and the scattering amplitude of nuclei in the sample under investigation. Theses interferences can easily been observed as resonances in velocity spectra when one uses a time integrated method. They can also been observed as quantum beats, when one would use the time differential method. For both methods it is important that one uses a reference sample and therefore both methods disserved the name “heterodyne methods.” As theses interferences are a product of two scattering amplitudes, the amplitude of a wave scattered form the investigated sample can be known with its phase. But it is assumed that the reference wave is known in advance by a proper choice of the reference sample. At first sight it is very likely that multiple scattering would add more complexity but in this paper it is claimed that on the contrary it provide a bonus, especially for single crystals. It provokes only a line broadening and a line shift of the resonances in the velocity spectra (or a change in the damping and frequency of the quantum beats when the time spectra are registered). Moreover these changes in the line shapes can easily be measured and they provide all the information needed to reconstruct a 3-D picture of the atomic arrangement of resonant nuclei and moreover they distinguish between different hyperfine sites. The method may be more practical for measurements on synchrotron radiation but it does also apply to velocity spectra obtained from resonant scattering with strong sources. The use of radioactive sources suffer from the disadvantage of poorer statistics or much longer accumulation times but they enjoy the advantage to be table-top and at-home experiments. As strong sources are now commercially available this possibility to measure not only the hyperfine fields but also the corresponding crystal structure could give a renewed impetus to the investigations with Moessbauer spectrometry, with “at home and table top” instrumentation.     

Solving the inverse transport problem in intergalactic space and determining the energy spectrum and composition of extragalactic sources of ultrahigh-energy particles

The propagation of ultrahigh-energy nuclei in an expanding Universe filled with background electromagnetic radiation is considered. A numerical method for solving the inverse problem for the equation of cosmic-ray transport is developed that allows the spectrum of sources to be determined from the cosmic-ray spectrum observed near the Earth. The spectra of injected protons and nuclei in extragalactic sources are found by assuming that they are functions of the magnetic rigidity of particles. The data from observations obtained in the Auger experiment are used.     

Inverse problem for the equation of ultrahigh energy cosmic ray transport

The propagation of ultrahigh energy nuclei in an expanding universe filled with background electromagnetic radiation is considered. A numerical method for solving the inverse problem for the equation of cosmic ray transport is developed. The method allows us to determine a source spectrum from the cosmic ray spectrum observed near Earth. The spectra of injected protons and nuclei of iron were found in extragalactic sources under the assumption that these types of particles predominate in the composition of the sources. The method of calculation is illustrated using observational data obtained in the Auger and Telescope Array experiments.     

Analysis of photoluminescence spectra of anthracene traces in photon traps

Photoluminescence spectra of small amounts of anthracene being in the photon trap, a specific type of the resonant cavity, were measured. In photon traps, radiation is input and output by optical waveguides. The use of ultraviolet light-emitting-diode sources of exciting radiation and a minipolychromator allowed photoluminescence spectra measurements in the range of 340–500 nm at an exposure of ～ 10^?3 s.     

靶等离子体真空紫外光谱研究

本文叙述了在靶等离子体实验装置上做的真空紫外区(500—2000)光谱实验。分析和研究了等离子体光谱,杂质成分、杂质来源和等离子体喷枪的发射机制。     

脉冲激光辐照液滴锡靶等离子体极紫外辐射的实验研究

采用波长13.5 nm的极紫外光作为曝光光源的极紫外光刻技术是最有潜力的下一代光刻技术之一, 它是半导体制造实现10 nm及以下节点的关键技术. 获得极紫外辐射的方法中, 激光等离子体光源凭借转换效率高、收集角度大、碎屑产量低等优点而被认为是最有前途的极紫外光源. 本文开展了脉冲TEA-CO₂激光和Nd:YAG激光辐照液滴锡靶产生极紫外辐射的实验, 对极紫外辐射的谱线结构以及辐射的时空分布特性进行了研究.实验发现: 与TEA-CO₂激光相比, 较高功率密度的Nd:YAG激光激发的极紫外辐射谱存在明显的蓝移; 并且激光等离子体光源可以认为是点状光源, 其极紫外辐射强度随空间角度变化近似满足Lambertian分布.     

Reference Spectra in the “Artificial-Moon” Scale and Cosmological Studies of Radio Sources

We present the modified version of the flux scale [1] of cosmic radio sources. The number of standard sources is increased, the dynamical range of the scale is extended by one order of magnitude toward weak fluxes, and the standard sources are distributed more uniformly over the northern hemisphere. The scale [1] at frequencies above 15 GHz is improved with allowance for additional data. New standard sources are determined in the millimeter wavelength range. The spectra of standard sources are obtained on the basis of accurate absolute measurements of the radiation flux density at frequencies 0.5-10 GHz by the method of an artificial moon. Spectrum shapes of the standard sources were determined by the method of relative spectra based on relative measurements in the frequency interval from 26 MHz to 31.4 GHz. This makes it possible to find spectra in the entire frequency range with an accuracy of 3-4%. We determined the spectra of more than 100 steep-spectrum extra-Galactic sources in the artificial-moon' scale. Most spectra have breaks in the frequency interval from 178 MHz to 14.9 GHz. The spectra of some sources have constant spectral indices. The distributions of the break frequencies of radio galaxies and quasars over celestial coordinates of these sources are obtained. These distributions are close to lognormal. The frequencies of the maxima of radio-galaxy and quasar distributions are equal to 1.25 and 2.5 GHz, respectively. The mean spectral indices as functions of frequency are determined for radio galaxies and quasars. The spectral indices of sources belonging to these two groups increase with frequency at the same rate below 3 GHz. At higher frequencies, the slope of the mean spectrum of galaxies remains the same, while the mean quasar spectrum flattens.     

Chemical shifts in Al—Si compounds by Zr Lα photo-electron spectrometry

The excitation of XPS spectra by Zr Lα radiation has the advantage that both the 1s peaks and their KLL Auger series are excited. This paper compares the peak positions, of metals, oxide and certain aluminosilicates, obtained using Zr Lα radiation and thus demonstrates a dependence of the Auger parameter on structures. This method of characterisation is particularly suitable for minerals such as silicates which are prone to charging, but is not possible for silicon with the conventional Mg and Al sources.