宇宙射线的地质作用

从宏观与微观两个角度分析了宇宙射线的地质作用，认为宇宙射线能量是地质作用一个不可忽视的因素     

The knee at cosmic ray spectra is explained due to interactions at the sources

In the paper the authors from the Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences in Beijing proposed a new model trying to explain the knee at cosmic ray spectra. The knee kept as a puzzle in cosmic ray physics for nearly half a century. The work was inspired by the recent observation of anomalous excess of electrons and positrons in cosmic rays. The work tries to explain the knee and the electron/positron excess in a single model.......     

宇宙线较长周期变化研究

利用羊八井ASγ阵列实验数据分析宇宙线的较长周期变化.收集整理Tibet ASγ阵列1994～2003年间记录的宇宙线触发率数据和气象数据,发现这段时间的宇宙线触发率存在明显的年周期变化,气压、室内温度、室外温度与宇宙线触发率有着相似的年变化,存在较强关联;对宇宙线触发率进行多元气象参量修正,修正后的宇宙线触发率不再有明显的年变化;利用小波分析和数学统计方法分析气象修正后的宇宙线触发率,没有发现确定的几日周期.统计结果显示：宇宙线周期变化中4日周期和6日周期较多,其次是5日7、日和8日周期.     

大科学装置与高能宇宙线起源的探索

大科学装置已经成为全球创新系统中具有支撑作用的框架结构,对中国作为一个国家和宇宙线物理作为一个研究领域来说也是一样的.在其一百年发展史中,传统的宇宙线研究并非完全以大科学装置为依托.20世纪80年代以后,为了探索宇宙中微子和极高能宇宙线粒子,那必不可少的巨大中微子灵敏体积和至少上千平方公里的极高能宇宙线探测面积才给这个古老的学科设定了新的标准,而随之提出的几个大科学装置相继建成并在近几十年的宇宙线研究的辉煌成就中占据了核心地位,尤其在甚高能伽马射线天文学.在过去的20年内,中国为发展巡天普查伽马射线源的广延空气簇射技术做出了巨大的努力,成功地运行了ASγ和ARGO-YBJ两个高海拔国际宇宙线实验.现在,我们提出独具特色的高海拔空气簇射测量装置LHAASO的建设计划,建设面积达一平方公里的复合探测器阵列,以多种探测手段的有机组合寻求发现高能宇宙线起源,挑战新世纪里未解之科学难题.凭借其30 TeV以上最高的探测灵敏度,LHAASO将成为整个宇宙线研究领域的支柱项目之一.     

Galactic cosmic ray origin of Li, Be and B in stars

A study of the implications of the hypothesis that high energy processes involving cosmic rays acting on the interstellar medium are the sources of the elements Li, Be and B present in stellar atmospheres and in the solar system.     

Detection and imaging of atmospheric radio flashes from cosmic ray air showers

The nature of ultrahigh-energy cosmic rays (UHECRs) at energies >10(20) eV remains a mystery. They are likely to be of extragalactic origin, but should be absorbed within approximately 50 Mpc through interactions with the cosmic microwave background. As there are no sufficiently powerful accelerators within this distance from the Galaxy, explanations for UHECRs range from unusual astrophysical sources to exotic string physics. Also unclear is whether UHECRs consist of protons, heavy nuclei, neutrinos or gamma-rays. To resolve these questions, larger detectors with higher duty cycles and which combine multiple detection techniques are needed. Radio emission from UHECRs, on the other hand, is unaffected by attenuation, has a high duty cycle, gives calorimetric measurements and provides high directional accuracy. Here we report the detection of radio flashes from cosmic-ray air showers using low-cost digital radio receivers. We show that the radiation can be understood in terms of the geosynchrotron effect. Our results show that it should be possible to determine the nature and composition of UHECRs with combined radio and particle detectors, and to detect the ultrahigh-energy neutrinos expected from flavour mixing.     

LHAASO实验中宇宙线次级粒子特性的模拟研究

高海拔宇宙线观测站(LHAASO)位于四川稻城海子山,海拔约4400 m,该实验采用多种手段,对进入大气层的宇宙线粒子进行精确的复合测量.高海拔区域,雷暴天气频繁,广延大气簇射中宇宙线次级粒子的数目、方向和能量都会受到雷暴电场的影响.本文利用Monte Carlo方法,模拟了宇宙线原初粒子进入大气层后的广延大气簇射过程,研究了次级粒子中光子、电子、μ子的纵向分布、横向分布和能量分布.结果表明,在LHAASO探测面,电子的数目比μ子多2～3倍、μ子横向分布范围比电子宽广、μ子的能量比电子大.若在雷暴期间,大气电场对电子(质量小、数目多)的影响将会更加明显.本工作对研究雷暴电场加速宇宙线次级带电粒子的物理机制具有重要意义,同时为理解地面实验的观测现象提供有用信息.     

小波分析在1-10TeV宇宙线时间变化研究中的应用

利用小波变换,结合折叠周期分析方法,对羊八井宇宙线观测站TibetASy阵列1997年11月到1998年6月的实验记录数据进行了周期分析,发现TeV和10TeV宇宙线流强中存在着太阳日和半太阳日周期变化．TeV宇宙线流强1d和0．5d周期变化的信噪比分别为9．8和12．9,其变化幅度分别为0．44-0．26％和0．3±0．18％,最大变化处的相位分别在约0．8（18h）和0．9（11h）．10TeV字宙线流强1d和0．5d周期变化的信噪比分别为10．1和12．9,其变化幅度分别约为0．5＋0．34％和0．35±0．23％,最大变化处的相位分别在约0．8（18h）和0．9（11h）．     

Relativistic ejecta from X-ray flash XRF 060218 and the rate of cosmic explosions

Over the past decade, long-duration gamma-ray bursts (GRBs)--including the subclass of X-ray flashes (XRFs)--have been revealed to be a rare variety of type Ibc supernova. Although all these events result from the death of massive stars, the electromagnetic luminosities of GRBs and XRFs exceed those of ordinary type Ibc supernovae by many orders of magnitude. The essential physical process that causes a dying star to produce a GRB or XRF, and not just a supernova, is still unknown. Here we report radio and X-ray observations of XRF 060218 (associated with supernova SN 2006aj), the second-nearest GRB identified until now. We show that this event is a hundred times less energetic but ten times more common than cosmological GRBs. Moreover, it is distinguished from ordinary type Ibc supernovae by the presence of 10(48) erg coupled to mildly relativistic ejecta, along with a central engine (an accretion-fed, rapidly rotating compact source) that produces X-rays for weeks after the explosion. This suggests that the production of relativistic ejecta is the key physical distinction between GRBs or XRFs and ordinary supernovae, while the nature of the central engine (black hole or magnetar) may distinguish typical bursts from low-luminosity, spherical events like XRF 060218.     

OLAM神经网络分析X荧光谱的预处理研究

在采用最优线性联想记忆(Optimal Linear Associative Memory)神经网络分析X荧光谱时,可用多种方式对谱作预处理,如去掉多余数据、取对数、横向压缩、标准化等.针对实验测得的水泥生料X荧光谱,分别用上述方法进行预处理,然后再用神经网络分析,与化学分析的偏差作对比.结果表明,去掉多余数据、横向压缩可以减少信息处理量,减少存储空间,提高运算速度,且对精度影响较小;标准化处理对含量较少的成分有优势,对含量大的成分误差太大;对数方法则不适用.     

小波分析在1-10TeV宇宙线气象效应研究中的应用

利用小波变换,结合折叠周期分析方法,对羊八井宇宙线观测站TibetASγ阵列1997年11月到1998年6月的实验记录数据进行周期分析,发现了气象参量,包括观测面处大气压和室外温度的日变化和半日变化.接下来的关联分析表明:宇宙线流强的周期变化与气压和温度的周期变化显著相关.     

GaSb薄膜结构的X射线衍射谱的精细分析

在GaAs单晶衬底上用分子束外延技术生长了GaSb薄膜,并用原子力显微镜和XRD技术分析了其结构特征.其结果可为生长优质的大失配太阳能电池材料提供一点参考.     

计算机辅助分子结构解析——有机化合物的红外谱图的解释

本文就计算机辅助有机化合物红外谱图解释的工作,结合作者用BASIC语言完成的IRSI-1程序,讨论了该程序的设计思想和介绍了总程序流程,最后对一个例子进行了剖析。