共查询到16条相似文献,搜索用时 93 毫秒
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利用基于Geant4建立起来的针孔成像模型获得了不同偏移量下γ与中子的好事例、能量沉积的比值,并模拟分析了强γ背景对中子针孔成像点扩展函数的影响。研究结果表明:在偏移量小于1 cm时,γ与中子的好事例之比、γ与中子的能量沉积峰值之比以及γ与中子的能量沉积总和之比分别在0.40~0.42,0.63~0.65以及0.46~0.49之间;偏移量大于1 cm时,比值下降明显,γ对中子的影响减小。在同一偏移量下,γ射线的点扩展函数的分布范围要比中子的小,两者叠加后所获得的点扩展函数的分布范围介于两者之间。在一定入射偏移范围内的成像质量优于在针孔中心位置入射时的成像质量。 相似文献
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采用蒙特卡罗方法对中子针孔成像系统进行了点扩展函数(PSF)的模拟研究, 利用高斯拟合的数学方法分析比较了几种不同条件下该系统的PSF。 研究结果表明, 在偏离量较小时, 利用高斯拟合得到的中子针孔成像系统的PSF是可行的, 而采用挡板可以很显著地减少拟合误差和提高其空间分辨率。 The point spread function (PSF) of a pinhole imaging system for fast neutron has been studied through Monte Carlo method. The PSFs under different conditions have been obtained and analyzed by fitting the simulating data with Gauss function. As the results show, when the excursion is little, the PSF obtained by Gauss function fitting is feasible. A baffle will reduce the error and improve the spatial resolution remarkably. 相似文献
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为了提高平面光栅成像系统的点扩展函数(PSF)提取准确度,构建PSF模型,提出一种基于Boltzmann函数的刃边函数拟合方法。构建以入射角为自变量的双曲线型变化PSF模型,揭示了光栅成像系统PSF的分布规律。最后,采用Lucy-Richardson算法对不同模糊程度的图像进行复原,并对复原后的图像进行质量评价,其中灰度平均梯度(GMG)提升均在60.2%以上,结构相似度(SSIM)提升均在66.5%以上。对比不同拟合方法的复原效果,结果表明,所提方法在对像差较大的图像进行复原时,效果明显优于其他同类方法,建立的PSF模型也可以准确地表现光栅成像系统的特性。 相似文献
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Hidekazu Takano Shigeki Konishi Takahisa Koyama Yoshiyuki Tsusaka Satoshi Ichimaru Tadayuki Ohchi Hisataka Takenaka Yasushi Kagoshima 《Journal of synchrotron radiation》2014,21(2):446-448
The experimental procedure for obtaining the point spread function (PSF) of a focusing beam generated using an X‐ray multilayer zone plate (MZP) with a narrow annular aperture has been developed. It was possible to reconstruct the PSF by applying the tomographic process to the measured dataset consisting of line spread functions (LSFs) in every radial direction on the focal plane. The LSFs were measured by a knife‐edge scanning method of detecting scattered intensity. In the experimental work, quasi‐monochromatic undulator radiation with a first harmonic energy of 20 keV was directly focused without a monochromator by the MZP, and the PSF was measured using this procedure. As a result, a near diffraction‐limited focused beam size of 46 nm full width at half‐maximum was obtained. 相似文献
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除中子外,聚变核心同时释放大量高能伽马,其能谱可反映聚变过程的关键物理参数,并为过程诊断提供重要信息.由于聚变伽马的时间与能量特性,需要设计高探测效率及能量分辨率的伽马谱仪.根据高能伽马谱仪的概念设计(gamma-to-electron magnetic spectrometer),针对该系统中伽马-电子转换靶、电子偏转汇聚、电子探测等关键环节进行优化设计以提高系统探测效率及能量分辨率.其中采用Monte-Carlo程序Geant4模拟研究了伽马-电子转换靶中康普顿散射与多次库仑散射对由转换靶出射电子的能谱与角分布的影响.开发并行遗传算法对复杂几何偏转磁场参数进行优化,得到低强度(小于100 Gauss)复杂边界偏转磁场.根据系统优化设计结果,采用Geant4模拟了该系统对不同能量伽马的响应.此外,还可模拟该系统对特征聚变伽马能谱的测量,结果显示,该系统可在聚变中子产额分别为2.5×10~(15)及1.2×10~(16)条件下,对10—20 MeV高能伽马能谱测量实现能量分辨分别满足0.5 MeV(小于5%)及0.25 MeV(小于2.5%),说明该系统可用于聚变过程伽马能谱的诊断. 相似文献
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The design of aperture weightings in ultrasound arrays is a multi-objective optimization problem, involving parameters such as delays, aperture size, focal depth, operating frequency and beam properties. Besides, apodization causes the SNR in array output to be decreased. We introduce an analytic expression of the lateral point spread function and a model for SNR as nonlinear functions of weights, based on which, a new aperture design method is established, resulting in an optimal set of weights. These weights provide a point spread function having the predetermined peak sidelobe level, while the SNR in array output is optimized. Optimization results from a linear array with M=128 elements equally spaced at one wavelength, center frequency f0=3.5 MHz and 50% relative bandwidth, have shown that decreasing the peak sidelobe level, decreases the SNR. Therefore, an array designer can select a proper set of weights according to its application, using a SNR curve versus to the peak sidelobe level. In addition, the method can maintain the same beam properties over a long range with low variations in the SNR. Simulation results have shown only 1 dB variations in the SNR for depths from 20 mm to 120 mm, which is a longer range and better SNR performance than the conventional methods. 相似文献
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Andreja Gomboc 《Contemporary Physics》2013,54(4):339-355
Gamma Ray Bursts are unpredictable and brief flashes of gamma rays that occur about once a day in random locations in the sky. Since gamma rays do not penetrate the Earth's atmosphere, they are detected by satellites, which automatically trigger ground-based telescopes for follow-up observations at longer wavelengths. In this introduction to Gamma Ray Bursts we review how building a multi-wavelength picture of these events has revealed that they are the most energetic explosions since the Big Bang and are connected with stellar deaths in other galaxies. However, in spite of exceptional observational and theoretical progress in the last 15 years, recent observations raise many questions which challenge our understanding of these elusive phenomena. Gamma Ray Bursts therefore remain one of the hottest topics in modern astrophysics. 相似文献