Ultrahigh energy cosmic ray deflection by the intergalactic magnetic field

被引：6

作者：

Aramburo-Garcia, Andres ^{[1
]}

Bondarenko, Kyrylo ^{[2
,3
]}

Boyarsky, Alexey ^{[1
]}

Nelson, Dylan ^{[4
]}

Pillepich, Annalisa ^{[5
]}

Sokolenko, Anastasia ^{[6
]}

机构：

[1] Leiden Univ, Inst Lorentz, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands

[2] CERN, Theoret Phys Dept, CH-1211 Geneva 23, Switzerland

[3] LEcole Polytech Fdrale Lausanne, CH-1015 Lausanne, Switzerland

[4] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany

[5] Max Planck Inst Astron, Knigstuhl 17, D-69117 Heidelberg, Germany

[6] Austrian Acad Sci, Inst High Energy Phys, Nikolsdorfergasse 18, A-1050 Vienna, Austria

来源：

PHYSICAL REVIEW D | 2021年 / 104卷 / 08期

基金：

欧洲研究理事会; 奥地利科学基金会;

关键词：

SIMULATING GALAXY FORMATION; ILLUSTRISTNG SIMULATIONS; SCALE ANISOTROPY; NUCLEI;

D O I：

10.1103/PhysRevD.104.083017

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The origin and composition of ultrahigh energy cosmic rays (UHECRs) remains a mystery. The common lore is that UHECRs are deflected from their primary directions by the Galactic and extragalactic magnetic fields. Here we describe an extragalactic contribution to the deflection of UHECRs that does not depend on the strength and orientation of the initial seed field. Using the IllustrisTNG simulations, we show that outflow-driven magnetic bubbles created by feedback processes during galaxy formation deflect approximately half of all 10(20) eV protons by 1 degrees or more, and up to 20 degrees-30 degrees. This implies that the deflection in the intergalactic medium must be taken into account in order to identify the sources of UHECRs.

引用

页数：6

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