Ultrahigh energy nuclei in the turbulent Galactic magnetic field

被引：46

作者：

Giacinti, G. ^{[1
,2
]}

Kachelriess, M. ^{[3
]}

Semikoz, D. V. ^{[2
,4
]}

Sigl, G. ^{[1
]}

机构：

[1] Univ Hamburg, Inst Theoret Phys 2, Hamburg, Germany

[2] APC, Paris, France

[3] NTNU, Inst Fys, Trondheim, Norway

[4] Russian Acad Sci, Inst Nucl Res, Moscow, Russia

来源：

ASTROPARTICLE PHYSICS | 2011年 / 35卷 / 04期

关键词：

Ultrahigh energy cosmic rays; Galactic magnetic fields; LARGE-SCALE STRUCTURE; COSMIC-RAYS; ROTATION MEASURES; MILKY-WAY; DEFLECTIONS;

D O I：

10.1016/j.astropartphys.2011.07.006

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this work we study how the turbulent component of the Galactic magnetic field (GMF) affects the propagation of ultrahigh energy heavy nuclei. We investigate first how the images of individual sources and of the supergalactic plane depend on the properties of the turbulent GMF. Then we present a quantitative study of the impact of the turbulent field on (de-)magnification of source fluxes, due to magnetic lensing effects. We also show that it is impossible to explain the Pierre Auger data assuming that all ultrahigh energy nuclei are coming from Cen A, even in the most favorable case of a strong, extended turbulent field in the Galactic halo. (C) 2011 Elsevier B.V. All rights reserved.

引用

页码：192 / 200

页数：9