论文部分内容阅读
太阳中子事件是与耀斑活动相关的偶发性即刻粒子事件,主要表现为地面宇宙线探测装置的计数瞬时突增.太阳中子携带着爆发源区的物理信息:耀斑大气的元素组成、大气高度、磁场的会聚程度以及磁流体湍动等.相对于其他带电粒子,中子能够不受太阳磁场和行星际磁场的束缚而直达地面.目前,对太阳中子事件的理论研究,主要是通过蒙特卡罗模拟,考虑太阳耀斑环中磁场的螺旋角散射作用和磁镜效应,计算耀斑磁环模型里各向异性中子的产生与太阳大气高度、时间、角度和能量间的关系,计算逃逸中子的角分布和能谱,以及逃逸到地球附近中子的能谱.观测方面,主要是结合地面中子监测器记录的超出时间与空间探测到的γ射线核谱线发射峰值的时间差,利用飞行时间方法(Time of Flight Method),考虑中子监测器的探测效率和中子在地球大气中的衰减因素,反演日面处的中子能谱.本文依据已确定的10例太阳中子事件,评述基本的观测特征,介绍相应的观测仪器,探讨太阳中子能谱计算的两种方法(观测法和模型法),比较不同方法获得的计算结果;并依托羊八井太阳宇宙线探测装置(中子监测器、太阳中子望远镜),报道对太阳中子的初步交叉探测特征(1998年11月28日GLE事件和2005年1月20日GLE事件),指出目前亟待解决的问题.
The solar neutron event is an incidental, immediate particle event associated with flare activity, which is mainly characterized by a sudden increase in the count of ground cosmic ray detection devices. The neutron carries the physical information of the source region of the flare: the elemental composition of the flare atmosphere, the height of the atmosphere , The degree of magnetic field convergence and magnetic fluid turbulence etc. Compared with other charged particles, neutrons can reach the ground without being bound by the solar magnetic field and the interplanetary magnetic field.At present, the theoretical study of the solar neutron event is mainly through the Monte- Carlo simulation, considering the helix angle scattering effect and the magnetic mirror effect of the magnetic field in the solar flare ring, the relationship between the generation of anisotropic neutrons in the flare magnetic ring model and the height, time, angle and energy of the solar atmosphere is calculated, Angle distribution and energy spectrum of the son, as well as the energy spectrum escaping to the neutrons near the earth.On the observational aspect, the time difference between the emission peak of the γ-ray nuclear line detected by the time and space detected by the ground neutron monitor is mainly used, The Time of Flight Method, taking into account the detection efficiency of neutron detectors and the attenuation of neutrons in the Earth’s atmosphere, Neutron spectrum.This paper reviews the basic observation features based on the 10 solar neutron events that have been identified, introduces the corresponding observation instruments, discusses two methods (observation method and model method) for calculating the solar neutron spectrum, Method; and relying on the Yangbajain solar cosmic ray detection device (neutron monitor, solar neutron telescope) to report the preliminary cross-detection characteristics of solar neutrons (GLE events of November 28, 1998 and 2005 January 20 GLE incident), pointing out the immediate problems to be solved.