Possibility of multi-TeV secondary gamma rays from GRB221009A

被引：0

作者：

Kalashev, Oleg ^{[1
,2
]}

Aharonian, Felix ^{[3
,4
,5
]}

Essey, Warren ^{[6
]}

Inoue, Yoshiyuki ^{[7
,8
,9
]}

Kusenko, Alexander ^{[6
,9
]}

机构：

[1] Ecole Polytech Fed Lausanne, Lab Astrophys, CH-1015 Lausanne, Switzerland

[2] Russian Acad Sci, Inst Nucl Res, 60th October Anniversary Prospect 7a, Moscow 117312, Russia

[3] Dublin Inst Adv Studies, Sch Cosm Phys, 31 Fitzwilliam Pl, Dublin, Ireland

[4] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany

[5] Yerevan State Univ, 1 Alek Manukyan St, Yerevan 0025, Armenia

[6] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA

[7] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan

[8] RIKEN, Interdisciplinary Theoret & Math Sci Program iTHEM, 2-1 Hirosawa, Saitama 3510198, Japan

[9] UTIAS Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan

来源：

PHYSICAL REVIEW D | 2025年 / 112卷 / 02期

基金：

日本学术振兴会;

关键词：

EXTRAGALACTIC BACKGROUND LIGHT; INTERGALACTIC MAGNETIC-FIELD; BLAZAR PKS 1424+240; ENERGY COSMIC-RAY; FERMI-LAT; TIME; CONSTRAINTS; DISCOVERY; EMISSION; SPECTRUM;

D O I：

10.1103/q7pf-d1k9

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The brightest gamma ray burst (GRB) ever observed, GRB221009A, produced a surprisingly large flux of gamma rays with multi-TeV energies, which are expected to be absorbed in interactions with extragalactic background light (EBL). If the highest energy gamma rays were produced at the source, their spectral shape would have to exhibit a nonphysical spike even for the lowest levels of EBL. We show that, for widely accepted models of EBL, the data can be explained by secondary gamma rays produced in cosmic ray interactions along the line of sight, as long as the extragalactic magnetic fields along the line of sight are 10-16 G or smaller, assuming 1 Mpc correlation length. Our interpretation supports the widely held expectation that GRB jets can accelerate cosmic rays to energies as high as 10 EeV and above, and it has implications for understanding the magnitudes of extragalactic magnetic fields.

引用

页数：7

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