Ultra-high-energy cosmic rays from low-luminosity active galactic nuclei

被引：8

作者：

Dutan, Ioana ^{[1
,2
,3
]}

Caramete, Laurentiu I. ^{[1
,2
,3
]}

机构：

[1] Inst Space Sci, Bucharest 077125, Romania

[2] Res Ctr Atom Phys & Astrophys, Bucharest 077125, Romania

[3] Max Planck Inst Radio Astron, D-53121 Bonn, Germany

来源：

ASTROPARTICLE PHYSICS | 2015年 / 62卷

关键词：

Cosmic ray; UHECR; AGN; Jet; Auger; RELATIVISTIC MAGNETOHYDRODYNAMIC SIMULATIONS; BLACK-HOLE; MAGNETIC-FIELD; ACCRETION DISK; JET FORMATION; ULTRARELATIVISTIC SHOCKS; PARTICLE-ACCELERATION; SYNCHROTRON EMISSION; RADIO; GALAXIES;

D O I：

10.1016/j.astropartphys.2014.09.007

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We investigate the production of ultra-high-energy cosmic ray (UHECR) in relativistic jets from lowluminosity active galactic nuclei (LLAGN). We start by proposing a model for the UHECR contribution from the black holes (BHs) in LLAGN, which present a jet power P-j <= 10(46) erg s(-1). This is in contrast to the opinion that only high-luminosity AGN can accelerate particles to energies >= 50 EeV. We rewrite the equations which describe the synchrotron self-absorbed emission of a non-thermal particle distribution to obtain the observed radio flux density from sources with a flat-spectrum core and its relationship to the jet power. We found that the UHECR flux is dependent on the observed radio flux density, the distance to the AGN, and the BH mass, where the particle acceleration regions can be sustained by the magnetic energy extraction from the BH at the center of the AGN. We use a complete sample of 29 radio sources with a total flux density at 5 GHz greater than 0.5 Jy to make predictions for the maximum particle energy, luminosity, and flux of the UHECRs from nearby AGN. These predictions are then used in a semi-analytical code developed in Mathematica (SAM code) as inputs for the Monte-Carlo simulations to obtain the distribution of the arrival direction at the Earth and the energy spectrum of the UHECRs, taking into account their deflection in the intergalactic magnetic fields. For comparison, we also use the CRPropa code with the same initial conditions as for the SAM code. Importantly, to calculate the energy spectrum we also include the weighting of the UHECR flux per each UHECR source. Next, we compare the energy spectrum of the UHECRs with that obtained by the Pierre Auger Observatory. (C) 2014 Elsevier B.V. All rights reserved.

引用

页码：206 / 216

页数：11

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