宇宙线高能粒子与液体闪烁体的核相互作用

利用放置在海拔3185米处的多板云室,以液体闪烁体作靶,研究宇宙线高能粒子产生的核相互作用。本文分析了18个由荷电粒子引起的核作用事例,用Castagnoli公式求得初能平均值E₀=(41±8)Bev,荷电粒子平均多重性n_s=4.9±0.3,以x=lgγ_ctgθ_l为变量作次级粒子的角分布,发现dN/dx分布可能存在着两个峯,文中试用二心模型对此角分布进行了讨论。 关键词：     

活动星系核与高能宇宙线

宇宙线发现100年来,人们对其成分、产生和加速机制、及其传播效应进行了广泛的研究,并获得了丰富的天体物理信息,但其起源至今仍然不清楚。一般认为相对低能的宇宙线起源于银河系内,极高能宇宙线起源于河外,而作为宇宙中最明亮的河外天体,活动星系核很可能是河外宇宙线源。随着多信使观测时代的到来,我们拥有了前所未有的从整体上去理解高能伽马射线和河外极高能宇宙线最好机遇。本文将简要地回顾和讨论活动星系核与高能宇宙线起源之间的关系,并对我国即将建成的高海拔宇宙线观测站（LHAASO）研究预期进行展望。     

活动星系核与高能宇宙线

 宇宙线发现100年来，人们对其成分、产生和加速机制、及其传播效应进行了广泛的研究，并获得了丰富的天体物理信息，但其起源至今仍然不清楚。一般认为相对低能的宇宙线起源于银河系内，极高能宇宙线起源于河外，而作为宇宙中最明亮的河外天体，活动星系核很可能是河外宇宙线源。随着多信使观测时代的到来，我们拥有了前所未有的从整体上去理解高能伽马射线和河外极高能宇宙线最好机遇。本文将简要地回顾和讨论活动星系核与高能宇宙线起源之间的关系，并对我国即将建成的高海拔宇宙线观测站（LHAASO）研究预期进行展望。     

太阳宇宙线耀斑中的甚高能粒子发射

对1972年8月在海拔3200m高山上利用大型云室组研究甚高能核作用的数据,进行了日计数率随时间变化的分析研究,发现在8月4日和8月7日两个大的太阳质子耀斑期间,事例计数率高出邻近期间日平均计数率的标准偏差三倍.其相应的初级宇宙线能量为10¹³eV左右.     

太阳宇宙线耀斑中的甚高能粒子发射

对1972年8月在海拔3200m高山上利用大型云室组研究甚高能核作用的数据,进行了日计数率随时间变化的分析研究,发现在8月4日和8月7日两个大的太阳质子耀斑期间,事例计数率高出邻近期间日平均计数率的标准偏差三倍。其相应的初级宇宙线能量为10~(13)eV左右.     

高能重离子碰撞中末态粒子的极角分布

在反应平面内不同极角方向为z轴的质心坐标系中,分析了末态粒子方向角分布的非对称性,建立了一种确定集合侧向流流角的方法.在以流方向为z轴的质心坐标系中研究了Bevalac流光室1.2AGeV Ar+KCl、1.2AGeV Ne+NaF和2.1AGeV Ne+NaF三种反应中末态粒子的极角分布,对末态粒子非对称发射部分所占的比例及其在流方向的集中程度做出了定量的估计.     

宇宙线和高能天体物理

羊八井中日合作二期阵列在1997-1998年最有意义的实验结果主要来自于把探测阈能降低到～3TeV的局部加密阵列部分。例如,在活动星系核MrK 501在1997年3月到8月变得比蟹状星云还亮很多的甚高能γ射线爆发期间，羊八井加密阵列与国际上七个大型契仑可夫望远镜一道看到了这个过程，而且是其中唯一有较完整的时变曲线的一家。同时，对蟹状星云的观测数据也显示在3TeV附近存在～4σ的γ流超出，而在10TeV则未观测到有统计意义的超出(最终结果将在1999年发表)。     

宇宙线高能族事例中簇射粒子的横向分布

对甘巴拉山铅乳胶室实验所获取的总观测能为100TeV至400TeV的高能族事例中簇射粒子的横向分布进行了分析,并与相应的Monte Carlo模拟计算进行了比较.模拟计算采用的是CORSIKA程序,其中的强相互作用采用QGSJET模型.结果表明:采用CORSIKA(QGSJET)程序进行模拟所给出的族事例中簇射粒子的横向分布以及族事例能量集中率分布的整体趋势均与相应的实验数据基本相符.     

ON THE INELASTICITY OF SUPERHIGH ENERGY COSMIC RAY INTERACTIONS

The inelasticity of p-air and A-air interactions of superhigh energy cosmic rays is analysed and the influence of the nuclear collision geometry is investigated.     

光电子的初能量分布与角度分布

本文利用了Nottingham关於透射系数的经验公式,将DuBrige的不考虑反射效应的光电子初能量分布理论加以推广。由於详细地考虑了表面位垒对发射出来的电子所起的折射作用,因此不仅讨论了光电子的初能量分布与法线能量分布,而且也讨论了角度分布。这些讨论都假定发射面是理想的金属表面,没有碎鳞效应;金属内部的电子满足费密-狄喇克(Fermi-Dirac)统计分布;并假定入射光为固定强度的非偏振的单色光。本文中所获得的光电子初能量分布公式相当简单,而且比已往的理论更符合实验结果。光电子的角度分布曲线呈蛋状,大的一端向外,这舆Ives的实验结果相符。如果表面的反射效应不存在,那么角度分布满足馀弦定律。其他如光电流的光谱分布、球形电容器(其中心的小电极为光电阶极)在阻滞场下的伏-安特性曲线的理论公式,以及法线能量分布和理想平行板电容器在阻滞场下的电压-雷流特性曲线的理论公式也都曾加以讨论。     

原子核电荷分布半径及结合能

从分析各方面实验结果(高能电子被核散射,μ—介原子的X谱)表明原子核电荷分布半径R_p很接近于和z^1/3成正比(R_p=r_opz^1/3。按照这看法修改了原子核结合能半经验公式(Bethe-Weizs?cker公式),把原来公式中库仑能项3/5 (z²e²)/r_pA^1/3)=a₃z²/A^1/3换成3/5 (z²e²)/r_opz^1/3) =a′₃z^5/3,结果改进了公式与实验符合的程度,并且按照新公式可以很正确地计算各元素中对β衰变最稳定的同位素的质量数。     

MEASUREMENT OF HEAVY PARTICLE MASS DISTRIBUTION IN COSMIC RAY AT SEA-LEVEL

The apparatus consisting of two time of flight systems and absorber and its performences are described. This apparatus has been used to measure heavy particle (p, d, and α) mass distribution in cosmic ray at sea-level, and the results compared with other works are given.     

HIGH ENERGY HADRONS IN ATMOSPHERIC COSMIC RAYS OBSERVED WITH Fe EMULSION CHAMBERS

A part of K4(1984—1985) Fe emulsion chambers exposed at Mt.Kanbala (5500m,atmospheric depth 520g/cm²)by China-Japan Emulsion Chamber Collaboration has been analyzed with systematic scanning and measurement.The distribution of the starting of the starting point depths of the observed showers is given.The zenith angle distribution,vertical intensity,energy spectrum and attenuation length of hadrons in air and in iron are presented.Our results are compared with the recent data given by other experiments,and they are consistent with each other approximately.     

INFORMATION ABOUT SUBQUARK FROM EXPERIMENTS ON SUPERNIGH ENERGY COSMIC RAY

In this paper a kind of fireball model for subquark stratum is proposed, which can be used to explain the cosmic ray experiments for superhigh energy range, e. g., the mean multiplicity of secondary particles increases as S increases average transversal momentum ⊥> increases as S increases …etc. It can also give predictions which can be verified experimentally. This means that the information of the existence of subquark can be probed in the experiments on superhigh energy cosmic ray. Furthermore, this also means that some new phenomena observed in the experiments. on superhigh energy cosmiq ray provide. probably this kind of information.     

HIGH ENERGY CLUSTER SCATTERING THEORY OF MANY PARTICLES SYSTEM

Within the framework of the Glauber theory, we divide the many particle systeminto two subsystems formed. by the "valence" particles and "sea" particles respective-ly. Then the multiple scattering amplitudes can be divided into "sea","sea","sea","valence", "valence","sea", and "valence","valence" multiple scattering amplitude.For the calculations of these different amplitudes different effective approximatemethods are proposed, Finally, for "sea"."sea". "sea""valence", "valence" "sea"and "valence"."valence" processes, we obatain the respective S-matrices which phy-sically clear and convenient in calculation.     

RESEARCH FOR THE POSSIBILITY ON DETECTING COSMIC RAY PARTICLES BY ACOUSTIC WAY

The exploring results of the possibility on detecting cosmic ray particles by acoustic way are reported. It shows that the ultrasonic background noise is very complicated and there are some individual and transient ultrasonic signals in the natural wide water. The mechanism producing these signals may be the sound radiation of the microbubbles in water. There is no evidence for the possible correlation between these signals and cosmic ray particles. The threshold energy of acoustic detection of EAS core is above 3﹒10¹⁶eV at sealevel and the threshold energy of acoustic detection of the local showers produced by cosmic ray particles is above 10¹⁴eV     

NUCLEAR CHARGE DISPERSION OF FRAGMENTS IN HIGH ENERGY PROTON-NUCLEUS COLLISION

The charge dispersion of fragments in high energy p+Cu,Kr and Xe reactions are calculated by statistical model and Monte Carlo technique.The corresponding data are reproduced quite well.It is shown that the charge dispersions are all nearly gaussian.The mass dependence of the most probable fragment charge reflects the rest target memory effect.