Examination of the model of supernovae origin of galactic cosmic rays by the theory of nucleosynthesis and by observations of TeV gamma-ray emission

从能量学、激波加速机制和银河宇宙线源的化学组成等方面的一般性争论来看，超新星遗迹（SNRs）被广泛认为是银河宇宙线（GCR）的主要来源。在这个项目中，我们从理论和实验两方面研究了这种情况，发现银河系宇宙射线源的成分在1.6倍内再现为Ia型和II型超新星的新鲜喷出物、被喷出物卷起的星际物质和沃尔夫-拉叶星风物质的混合物。根据最近的超新星核合成模型，确定了四种源物质的最佳混合比。作为奖励，用CANGAROO 3.8 m大气切伦科夫望远镜观测了壳型SNRXJ1713.7 -3946，获得了TeV γ-γ的证据。X射线辐射来自遗迹的NW边缘，统计学显著性为0.56。数据表明，发射区域比望远镜的点扩展函数要宽得多。发射的程度与ASCA观察到的硬X射线一致。这种TeV的伽马射线辐射可以归因于冲击加速的超相对论电子对宇宙微波背景辐射的逆康普顿散射。在这个假设下，一个相当低的磁场为1011微高斯的剩余推导。

Supernova remnants (SNRs) are widely believed to be a major source of galactic cosmic rays (GCRs) from the general arguments on energetics, shock acceleration mechanisms, and the chemical composition of the source of GCR. In this project, we examined this scenario both theoretically and experimentally.It is found that the galactic cosmic ray source composition is reproduced within a factor of 1.6 as a mixture of fresh ejecta of Type Ia and Type II supernovae, the interstellar matter which is swept up by the ejecta, and Wolf-Rayet stellar wind material. The best mixing ratio of the four source materials are determined on the basis of the recent nucleosynthetic models of supernovae. As a bonus, the frequency of occurrence of SNIa relative to SNII and acceleration time of the GCRs after SNe explosions are estimated with the best mixing ratios to be 〜0.43 and 〜1000 y respectively.We observed the shell type SNR RX J1713.7-3946 with CANGAROO 3.8 m atmospheric Cerenkov telescope and obtained evidence for TeV gamma-ray emission from the NW rim of the remnant with 〜5.6 statistical significance. The data indicate that the emitting region is much broader than the point spreading function of the telescope. The extent of the emission is consistent with that of hard X-rays observed by ASCA. This TeV gamma-ray emission can be attributed to the Inverse Compton scattering of the Cosmic Microwave Background radiation by shock accelerated ultra-relativistic electrons. Under this assumption, a rather low magnetic field of 〜11 microgauss is deduced for the remnant.