High-energy cosmic rays from supernovae in young clusters of massive stars

被引：0
作者：
Bykov, A. M. [1 ,2 ,3 ]
Ellison, D. C. [4 ]
Kalyashova, M. E. [1 ]
Osipov, S. M. [1 ]
机构：
[1] Ioffe Inst, St Petersburg 194021, Russia
[2] Peter Great St Petersburg Polytech Univ, St Petersburg, Russia
[3] Int Space Sci Inst, Bern, Switzerland
[4] North Carolina State Univ, Dept Phys, Box 8202, Raleigh, NC 27695 USA
来源：
RENDICONTI LINCEI-SCIENZE FISICHE E NATURALI | 2019年 / 30卷 / SUPPL 1期
基金：
俄罗斯科学基金会;
关键词：
Cosmic rays; modeling; Supernovae; Young massive stellar clusters; INTERSTELLAR; ACCELERATION; REMNANTS;
D O I：
10.1007/s12210-019-00788-7
中图分类号：
O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];
学科分类号：
07 ; 0710 ; 09 ;
摘要：
While the bulk of GeV-100 TeV cosmic rays (CRs) can be accelerated at the shock of the most common supernova remnants the problem of CR acceleration to and above the PeV regime is still an open issue. We give a brief discussion of the production of 100 PeV regime cosmic rays by supernovae in young compact clusters of massive stars. This implies a spatial and temporal correlation of the SNe in the cluster over similar to 107year\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\sim 10<^>7\,\hbox {year}$$\end{document} which may affect the high-energy CR anisotropy. Here, we discuss the temporal evolution of the dipole angular anisotropy of 300 PeV CR protons accelerated within young massive star clusters.
引用
收藏
页码：155 / 158
页数：4
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