High Energy Cosmic Rays from Fanaroff-Riley radio galaxies

被引：14

作者：

Eichmann, B. ^{[1
]}

机构：

[1] Ruhr Univ Bochum, RAPP Ctr, Inst Theoret Phys Plasma Astroteilchenphys 4, D-44780 Bochum, Germany

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2019年 / 05期

关键词：

active galactic nuclei; ultra high energy cosmic rays; cosmic ray theory; extragalactic magnetic fields; X-RAY; JET-POWER; ACCELERATION; SPECTRUM; LOBES; EMISSION; LIMIT;

D O I：

10.1088/1475-7516/2019/05/009

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The extended jet structures of radio galaxies (RGs) represent an ideal acceleration site for High Energy Cosmic Rays (HECRs) and a recent model showed that the HECR data can be explained by these sources, if the arrival directions of HECRs at energies less than or similar to 8 EeV from a certain RG, Cygnus A, are isotropized. First, this work introduces the inverted simulation setup in order to probe the isotropy assumption. Here, different extragalactic magnetic field models are compared showing that either a magnetic field of primordial origin that yields a high field strength in the large scale structures of the Universe is needed, or a significant contribution by a multitude of isotropically distributed sources. Secondly, the HECRs contribution by the bulk of RGs of different Fanaroff-Riley (FR) type is determined. Here, the most recent FR-type dependent radio-to-CR correlations Q(cr) proportional to L-radio(beta L) are used, and the impact of the slope beta(L) on the HECRs is analyzed in detail. Finally, it is carved out that FR-II RGs provide a promising spectral behavior at the hardening part of the CR flux, between about 3 EeV and 30 EeV, but most likely not enough CR power. At these energies, FR-I RGs can only provide an appropriate flux in the case of a high acceleration efficiency and beta(L)greater than or similar to 0.9, otherwise these sources rather contribute below 3 EeV. Further, the required acceleration efficiency for a significant HECR contribution is exposed dependent on beta(L) and the CR spectrum at the acceleration site.

引用

页数：20

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