Muographic imaging with a multi-layered telescope and its application to the study of the subsurface structure of a volcano

In conventional muography observations using two detectors for muon tracking, the accidental coincidence of vertical electromagnetic showers generates identical trajectories to the muon tracks. Although muography has favorable properties, which allow direct density measurements inside a volcano, the measured density is lower than the actual value due to these fortuitous trajectories. We performed muography of Usu volcano, and confirmed that, in comparison with a use of two detectors, background noise levels were reduced by more than one order of magnitude using seven detectors for selecting linear trajectories. The resultant muographic image showed a high-density region underneath the central region of Usu volcano. This picture is consistent with the magma intrusion model proposed in previous studies. To clarify the three-dimensional location and actual size of the detected high-density body, multidirectional muographic measurements are necessary.     

用羊八井太阳宇宙线探测装置对太阳耀斑中子的初步探测

羊八井的地理优势特别适合于对太阳耀斑中子的观测.中日双方合作在羊八井建造了太阳中子望远镜和中子监测器,准备在第23太阳活动周的峰年到来之际,对太阳耀斑中子进行观测.设备于1998年10月开始采集数据,并在1998年11月28日观察到伴随一次X3.3级耀斑的计数超出.本文报道初步的探测结果.     

羊八井太阳中子望远镜和中子监测器对2005年1月20日GLE事件的探测

西藏羊八井位于东经90.53°, 北纬30.11°, 海拔4310m, 垂直地磁截止刚度14.1GV. 2005年1月20日羊八井太阳中子望远镜和中子监测器探测到与X7.1/2b太阳耀斑相关的GLE事件, 其中太阳中子望远镜能量>40MeV的能道在5min(07:00—07:05UT)和20min(07:00—07:20UT)的时间间隔内计数率增长的统计显著性分别是3.7σ和6.0σ, 同时羊八井中子监测器也探测到计数率的增长,初始时间为06:51—06:52UT. 观测表明在这次GLE事件中太阳质子可被加速到能量大于10GeV.     

中国锦屏地下实验室缪子辐射环境蒙特卡罗方法模拟

用蒙特卡罗方法对中国锦屏地下实验室（CJPL）的缪子辐射本底进行了模拟。在对宇宙线缪子进行模拟时,依据海平面缪子流强Gaisser公式建立模型,并利用MUSIC程序,模拟了CJPL实验室的剩余缪子归一化能谱,进一步利用FLUKA程序模拟得到了缪致光子、中子的产额和平均能量。结果表明：剩余缪子的平均能量369 GeV,通量3.1710-6 m-2s-1,次级光子总的注量率约1.5710-4 m-2s-1,次级中子总的注量率约8.3710-7 m-2s-1。通过与世界上其他地下实验室本底水平的对比,表明CJPL的缪子辐射环境低于世界上大多数地下实验室。     

用银河宇宙线数据分析1991年3月24日CME的结构

依据CME到达磁层时会引起银河宇宙线强度的突然下降，利用小波分析方法确定宇宙线强度变化的突变时刻，判断CME到达磁层顶的时刻，从而得到这次CME在磁层顶附近的结构.分析结果表明，CME驱动的激波厚度约为02228AU，CME的前端到CME最强磁场结构的空间尺度约为0325AU． 关键词： CME 地磁暴 银河宇宙线 小波分析     

雷暴电场对宇宙射线次级粒子μ 子的影响研究

西藏羊八井宇宙射线观测站的中子监测器主要探测宇宙射线次级粒子中能量在500 MeV—20 GeV的核子成分和少量的负μ子成分. 本文分析了2008—2010年观测站附近发生的62次雷暴期间中子监测器和大气平均电场仪的同步观测资料, 发现27次雷暴期间中子监测器计数率发生明显变化, 显著性S>5σ, 其中13次变化显著, 显著性S>10σ . 显著性S>10σ的13次个例信号变化百分比与地面电场场强幅值之间存在大体一致的变化趋势, 而显著性在5σ <S<10σ之间的14次个例信号变化百分比与地面电场场强幅值之间不存在相似的变化趋势. 较强雷暴当顶时中子监测器计数率变化一般不明显, 而中子监测器计数率变化明显的个例则多发生于雷暴云不当顶, 但探测器仍处于雷暴云下部正电荷层的控制范围之内时, 或者当顶雷暴处于形成或消散阶段. Dorman等把雷暴期间中子监测器计数率的变化归因于雷暴云内电场对宇宙射线次级粒子μ子的作用, 并建立了雷暴期间中子监测器计数率变化与雷暴地面电场相关联的理论. 本文分析发现雷暴期间羊八井中子监测器计数率变化与地面电场场强之间相关性较小或者没有相关性, 不支持Dorman的理论.     

Characteristic variations in the effect of diluents on polymer crystallization and melting observed for a sample of poly(ethylene-co-octene)

Melting points in mixtures of a crystallizable polymer with a low-molar-mass diluent depend on both, the diluent fraction and the crystal thickness. A differentiation of the two factors can be achieved by temperature-dependent SAXS experiments. A corresponding study, complemented by DSC, dilatometry, microscopy and AFM-imaging, was carried out for mixtures of a poly(ethylene-co-octene) with n-C₁₆H₃₄, c-C₁₆H₃₂ and methyl-anthracene, respectively. All diluents lead for a constant crystal thickness to melting point depressions in agreement with Raoult's law. On the other hand, the effect of the diluents on the thickness of the crystals formed at a fixed crystallization temperature varies. While in the presence of the two alkanes thicker crystals form, no effect arises for the methyl-anthracene—as was previously found for the octene-co-units. We consider these observations as a further support for our view that polymer crystallization follows a multi-stage route which includes a passage through an intermediate mesomorphic phase. Under such conditions crystal thicknesses would only be affected if the diluent is still present in the mesomorphic phase and stay invariant if the diluent molecules are already rejected when this intermediate phase forms.