Numerical simulations of diffusive shock acceleration in SNRs

被引：50

作者：

Zirakashvili, V. N. ^{[1
]}

Ptuskin, V. S. ^{[1
]}

机构：

[1] Pushkov Inst Terr Magnetism Ionosphere & Radiowav, Troitsk 142190, Moscow Region, Russia

来源：

ASTROPARTICLE PHYSICS | 2012年 / 39-40卷

基金：

俄罗斯基础研究基金会;

关键词：

Cosmic rays; Acceleration; Supernova remnants; MAGNETIC-FIELD AMPLIFICATION; YOUNG SUPERNOVA-REMNANTS; COSMIC-RAY ACCELERATION; PARTICLE-ACCELERATION; STREAMING INSTABILITY; CASSIOPEIA-A; EMISSION; WAVES; INJECTION; SPECTRUM;

D O I：

10.1016/j.astropartphys.2011.09.003

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

A new numerical model of the nonlinear diffusive shock acceleration is presented. It is used for modeling of particle acceleration in supernova remnants. The model contains coupled spherically symmetric hydrodynamic equations and the transport equations for energetic protons, ions and electrons. The forward and reverse shocks are included in the consideration. The spectra of cosmic rays released into interstellar medium from a supernova remnant are determined. The role of the reverse shock in the production of cosmic ray ions and positrons is discussed. (C) 2011 Elsevier B.V. All rights reserved.

引用

页码：12 / 21

页数：10

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