适用于爆炸物CT检测重建图像去噪新算法

场旅客行李爆炸物CT检测成像过程中不可避免地受到噪声影响,对重建图像的去噪处理是爆炸物CT检测技术中的一个重要环节。针对机场旅客行李隐藏爆炸物快速检测、重建图像质量要求和引入的噪声特点,提出了一种有效的图像去噪算法将小波包分析与快速中值滤波相结合,并且对小波包系数运用一种新的阈值去噪方法。实验结果表明,该算法能更有效地去除重建图像的噪声并保持图像的边缘细节。     

Low threshold particle arrays

While atmospheric Cherenkov telescopes have a small field of view and a small duty fraction, arrays of particle detectors on ground have a 1 sr field of view and a 100% duty fraction. On the other hand, particle detector arrays have a much higher energy threshold and an inferior hadron rejection as compared to Cherenkov telescopes. Low threshold particle detector arrays would have potential advantages over Cherenkov telescopes in the search for episodic or unexpected sources of gamma rays in the multi-TeV energy range. Ways to improve the threshold and hadron rejection of arrays are shown, based on existing technology for the timing method (with scintillator or water Cherenkov counters) and the tracking method (with tracking detectors). The performance that could be achieved is shown by examples for both methods. At mountain altitude (about 4000 m or above) an energy threshold close to 1 TeV could be achieved. For any significant reduction of the hadronic background by selecting muon-poor showers a muon detection area of at least 1000 m² is required, even for a compact array.     

Theoretical studies of the flux and energy spectrum of gamma radiation from the Sun

The purpose of this work is to study the various -ray-production mechanisms in solar flares and to calculate the flux, the spectrum, and the decay curves of radiation. Using the continuity equation and taking into account the energy losses for solar-flare-accelerated particles, we obtain the time-dependent particle distribution and thus the time behavior of the resulting rays. The important processes for producing rays in solar flares are found to be nonthermal electron bremsstrahlung, decay of neutral mesons, positron annihilation, neutron capture, and decay of excited nuclei. The results are applied to several known solar flares. For a large flare such as the class 3⁺ on February 23, 1956, continuous rays with energies up to 100 MeV from electron bremsstrahlung and neutral meson decays are observable at the orbit of the Earth by existing -ray detectors. Line rays from positron annihilation (0.51 MeV), neutron capture (2.23 MeV), and deexcitation of excited nuclei O¹⁶ (6.14 and 7.12 MeV) and C¹² (4.43 MeV) are particularly strong and well above the continuous -ray background due to electron bremsstrahlung. These lines can be detected at the Earth.NASA-NRC Resident Research Associate.     

喷气动力装置的红外辐射源及其抑制

本文分析喷气动力装置的红外辐射源,并讨论抑制红外辐射的技术途径.喷气动力装置的红外辐射来源于燃烧引起的高温,并可区分为两大类:固体表面的辐射和热喷流的辐射.一般而言,抑制红外辐射可从以下三个方面着手:(1)用冷却或绝热的方法降低辐射表面的温度,或通过蔽挡阻止红外辐射的传播;(2)加速喷气流与周围空气的混合,使喷流温度快速降低;(3)降低燃烧产物中辐射成分的浓度.     

Radioisotope detection and identification at high speeds using passive sensors

A network of radiation sensors for the protection of a military base against radiological/nuclear threats has been integrated in a testbed. Two key subsystems of this network are the array of sensitive radiation detectors and the subsystem for notifying the operators of radiation events. The alarm/alert notification subsystem automatically issues notifications to the command post in real-time. The resulting reporting to the command post appears to be adequate for non-technical operational personnel. The CONOPS for the protection system relies on the sensitive detection and identification of all radioactive sources well before the transporting vehicles reach the base gates. This is a unique feature of this protection system. Discriminating sodium-iodide detectors, in conjunction with plastic scintillators and neutron detectors comprise a high-performance detection subsystem. The use of various correlation techniques has permitted the demonstration of the detection of source strengths of tens of /spl mu/Ci moving at highway speeds and at several meters separation. A companion algorithm identifies the detected radioisotope when sufficient counts are available.     

轴对称火焰温度场的全息干涉计量

本文对轴对称位相物体的全息干涉计量中光线在位相物体中的折射引起的计量误差进行了计算分析,并且介绍了一种修正这种误差的简单方法。根据这一原理对酒精灯火焰和氢气火焰的温度分布进行了全息干涉计量。在干涉条纹的细化搜索中,采用了计算机图像处理方法。      

TeV radiation from galactic sources

The detection of the Crab Nebula as a steady source of TeV gamma rays puts the field of Very High Energy Gamma-Ray Astronomy on a firm observational basis and permits a critical re-assessment of the claims for the detection of a multitude of episodic binary sources. A new generation of detectors in the TeV and PeV energy regions is coming on-line; together with the telescopes of the Gamma-Ray Observatory these instruments will present a new perspective on one of the last frontiers of astronomy.     

基于神经网络的CT图像重建方法研究

旅客行李隐藏爆炸物CT检测是机场安检的重要部分,图像重建是CT检测技术的重要环节,但实际中往往得不到完全的投影数据。针对不完全投影数据或数据量较少情况的重建问题,提出将神经网络算法应用于图像重建,并利用完全投影条件下FBP算法的重建结果作为网络的目标输出进行权值学习,从而降低网络结构和训练的复杂性。对该算法进行计算机模拟仿真试验,试验结果表明,该算法能有效地完成不完全投影数据的图像重建,且重建图像质量较高。     

Neutron Monitor Response Functions

The neutron monitor provides continuous ground-based recording of the hadronic component in atmospheric secondary radiation which is related to primary cosmic rays. Simpson (1948) discovered that the latitude variation of the secondary hadronic component was considerably larger than the muon component suggesting the response of a neutron monitor is more sensitive to lower energies in the primary spectrum. The different methods of determining the neutron monitor response function of primary cosmic rays are reviewed and discussed including early and recent results. The authors also provide results from a new calculation (Clem, 1999) including angle dependent yield functions for different neutron monitor types which are calculated using a simulation of cosmic ray air showers combined with a detection efficiency simulation for different secondary particle species. Results are shown for IGY and NM64 configurations using the standard ¹⁰BF₃ detectors and the new ³He detectors to be used in the Spaceship Earth Project (Bieber et al., 1995). The method of calculation is described in detail and the results are compared with measurements and previous calculations. A summary of future goals is discussed. This revised version was published online in August 2006 with corrections to the Cover Date.     

Cosmic Rays and Earth – A Summary

Cosmic rays provide a diagnostic tool to analyze processes in interplanetary space and at the Sun. Cosmic rays also directly affect the terrestrial environment and serve as indicators of solar variability and non anthropogenic climatic changes on Earth at present and in the distant past. After the invention of the neutron monitor by John A. Simpson in 1948, an international network of cosmic ray detectors developed in a cooperative effort to examine temporal and spatial variations in our space environment. The resulting datasets represent the longest continuous, high time resolution series of particle radiation measurement in space science. At present, the neutron monitor network is complemented by spacecraft instrumentation to study solar-terrestrial correlated phenomena. This revised version was published online in August 2006 with corrections to the Cover Date.     

Cosmic Rays in the Heliosphere: Requirements for Future Observations

Since the publication of Cosmic Rays in the Heliosphere in 1998 there has been great progress in understanding how and why cosmic rays vary in space and time. This paper discusses measurements that are needed to continue advances in relating cosmic ray variations to changes in solar and interplanetary activity and variations in the local interstellar environment. Cosmic ray acceleration and transport is an important discipline in space physics and astrophysics, but it also plays a critical role in defining the radiation environment for humans and hardware in space, and is critical to efforts to unravel the history of solar activity. Cosmic rays are measured directly by balloon-borne and space instruments, and indirectly by ground-based neutron, muon and neutrino detectors, and by measurements of cosmogenic isotopes in ice cores, tree-rings, sediments, and meteorites. The topics covered here include: what we can learn from the deep 2008–2009 solar minimum, when cosmic rays reached the highest intensities of the space era; the implications of ¹⁰Be and ¹⁴C isotope archives for past and future solar activity; the effects of variations in the size of the heliosphere; opportunities provided by the Voyagers for discovering the origin of anomalous cosmic rays and measuring cosmic-ray spectra in interstellar space; and future space missions that can continue the exciting exploration of the heliosphere that has occurred over the past 50 years.     

Intergalactic magnetic fields, and some connections with cosmic rays

An overview is presented of the methods of probing for the geometry, and strength of intergalactic magnetic fields. Recent results are briefly surveyed for galaxy halos, galaxy clusters, and the intergalactic medium on various scales, and some rele vant physical processes and radiation processes are mentioned, as well as the coupling between intergalactic magnetic fields and cosmic rays.The general trend of recent results indicates that, wherever we detect intergalactic hot gas and galaxies, we also find magnetic fields at levels of 10^–7 G, or higher. The hitherto undetected, weaker fields in the ratified i.g.m. and in large intergalactic voids could be probed by both Faraday rotation, and possibly using very energetic CR nuclei (> 10²⁰eV), and/or transient extragalactic ray bursts.     

The Energy Spectra and Anisotropies of Cosmic Rays

The existing paradigm of the origin of Galactic cosmic rays places strong supernovae shocks as the acceleration site for this material. However, although the EGRET gamma-ray telescope has reported evidence for GeV gamma rays from some supernovae, it is still unclear if the signal is produced by locally intense cosmic rays. Although non-thermal X-ray emissions have been detected from supernova remnants and interpreted as synchrotron emission from locally intense electrons at energies up to 100 TeV, the inferred source energy spectral slopes seem much steeper than the electron source spectrum observed through direct measurements. It remains the case that simple energetics provide the most convincing argument that supernovae power the bulk of cosmic rays. Two characteristics which can be used to investigate this issue at high energy are the source energy spectra and the source composition derived from direct measurements.     

空间目标红外辐射特性分析

研究空间目标的红外辐射特性,对于探测识别空间目标、监视空间碎片、保障卫星运行安全等问题有重要意义.本文以空间卫星为目标,分析了其红外辐射特性形成的原理,依据空间目标的热平衡方程,应用节点网络法求解目标表面的温度分布,并结合普朗克定律推导空间目标红外辐射度的计算方法,在分析总结相关资料的基础上得到了求解空间目标红外辐射特...     

Detection of iron lines in the persistent emission of some X-ray burst sources observed by EXOSAT

We have observed the X-ray burst sources 4U1728-33 and 4U1813-14 with the ME detectors aboard EXOSAT, and present here results of a spectral analysis of their persistent emissions. For both sources the data can be well fitted by a double blackbody continuum and a Gaussian emission line. The two spectral components can be interpreted in terms of a blackbody radiation from the neutron star, and emission from the inner part of an accretion disc. The line feature is consistent with the 6.7 keV iron emission line expected in the presence of a hot extended object (X-ray corona) around the neutron star.     

Gamma-hadron separation at high energies in view of recent cross section measurements

Recent measurements of the cross section for hadron photoproduction at HERA are reviewed and their importance for gamma ray astronomy is outlined. Various methods of distinguishing gamma and hadron primaries among cosmic rays in the air shower range are then discussed in view of our (insufficient) knowledge of the relevant hadron hadron cross sections. Theoretical model calculations indicate that the fraction of proton primaries mimicking gamma rays may be as high as one in a thousand.     

Hard rock cosmic ray archaeology

Recent examinations of extraterrestrial materials exposed to cosmic rays for different intervals of time during the geological history of the solar system have generated a wealth of new information on the history of cosmic radiation. This information relates to the temporal variations in

1. the flux and energy spectrum of low energy (solar) protons of ? 10 MeV kinetic energy;
2. the flux and energy spectrum of (solar) heavy nuclei of Z > 20 of kinetic energy, 0.5–10 MeV/n;
3. the integrated flux of protons and heavier nuclei of ? 0.5 GeV kinetic energy, and
4. the flux and energy spectrum of nuclei of Z > 20 of medium energy — 100–2000 MeV/n kinetic energy.

The above studies are entirely based on the natural detector method which utilises two principal cosmogenic effects observed in rocks, (i) isotopic changes and (ii) changes in the crystalline structure of rock constituents, due to cosmogenic interactions. The information available to date in the field of hard rock cosmic ray archaeology refers to meteorites and lunar rocks/soil. Additional information based on study of cosmogenic effects in man-made materials exposed to cosmic radiation in space is also discussed. It is shown that the natural detectors inspite of their extreme simplicity have begun to provide cosmic ray information in a very quantitative and precise manner comparable to the most sophisticated electronic particle detectors. The single handicap in using the hard rock detectors is however the uncertainty regarding their manner of exposure, geometry etc. At present, a variety of techniques are being used to study the evolutionary history of extraterrestrial materials and as this field grows, uncertainties in cosmic ray archaeology will correspondingly decrease.     

Stereoscopic measurements of the Čerenkov radiation produced by TEV gamma rays

Current approaches to the identification of VHE gamma rays using stereo images of erenkov light flashes are reviewed. The method of analysis developed by the University of Durham group involving a measure of cascade development is described. This method is applied to observations of a burst of VHE gamma rays from AE Aqr and enhancement of the gamma ray signal is demonstrated.     

La gamma astronomie

It is possible to predict the amount of gamma rays which are produced in various astronomical objects = gamma rays due to nuclear reactions, to bremsstrahlung, to cosmic rays, to annihilation of matter and anti-matter. These predictions are compared to the results of the observations with Explorer XI and are used to suggest new experiments. The following experiments are suggested:

1. (1)
   to measure the γ flash associated with Supernovae;