Particle spectra and mass composition in the ultra-high energy region in the framework of the Galactic origin of cosmic rays

The possibility for a self-consistent description of all the basic features of the observed cosmic ray spectra and primary composition variations in the energy range of 1015 ÷ 1020 eV within the Galactic origin scenario is examined. We assume the existence of Galactic sources that accelerate particl...

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Main Authors: Lagutin A.A., Volkov N.V., Tyumentsev A.G., Raikin R.I.
Format: Article
Language:English
Published: EDP Sciences 2017-01-01
Series:EPJ Web of Conferences
Online Access:https://doi.org/10.1051/epjconf/201714506004
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author Lagutin A.A.
Volkov N.V.
Tyumentsev A.G.
Raikin R.I.
author_facet Lagutin A.A.
Volkov N.V.
Tyumentsev A.G.
Raikin R.I.
author_sort Lagutin A.A.
collection DOAJ
description The possibility for a self-consistent description of all the basic features of the observed cosmic ray spectra and primary composition variations in the energy range of 1015 ÷ 1020 eV within the Galactic origin scenario is examined. We assume the existence of Galactic sources that accelerate particles up to ∼ 3 · 1018Z eV and take into account a highly inhomogeneous (fractal-like) distribution of matter and magnetic fields in the Galaxy that leads to extremely large free paths of particles (“Lévy flights”), along with an overwhelming contribution to the cosmic ray fluxes observed above ∼1018 eV from particles reaching the Solar System without scattering. Our scenario was refined on the basis of recent experimental results on primary mass composition. Model predictions, which could be verified with the improved high-precision measurements in the nearest future are discussed.
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spelling doaj.art-8bc944e6d897468b916fb64495280e432022-12-21T22:52:32ZengEDP SciencesEPJ Web of Conferences2100-014X2017-01-011450600410.1051/epjconf/201714506004epjconf-isvhecri2016_06004Particle spectra and mass composition in the ultra-high energy region in the framework of the Galactic origin of cosmic raysLagutin A.A.Volkov N.V.Tyumentsev A.G.Raikin R.I.The possibility for a self-consistent description of all the basic features of the observed cosmic ray spectra and primary composition variations in the energy range of 1015 ÷ 1020 eV within the Galactic origin scenario is examined. We assume the existence of Galactic sources that accelerate particles up to ∼ 3 · 1018Z eV and take into account a highly inhomogeneous (fractal-like) distribution of matter and magnetic fields in the Galaxy that leads to extremely large free paths of particles (“Lévy flights”), along with an overwhelming contribution to the cosmic ray fluxes observed above ∼1018 eV from particles reaching the Solar System without scattering. Our scenario was refined on the basis of recent experimental results on primary mass composition. Model predictions, which could be verified with the improved high-precision measurements in the nearest future are discussed.https://doi.org/10.1051/epjconf/201714506004
spellingShingle Lagutin A.A.
Volkov N.V.
Tyumentsev A.G.
Raikin R.I.
Particle spectra and mass composition in the ultra-high energy region in the framework of the Galactic origin of cosmic rays
EPJ Web of Conferences
title Particle spectra and mass composition in the ultra-high energy region in the framework of the Galactic origin of cosmic rays
title_full Particle spectra and mass composition in the ultra-high energy region in the framework of the Galactic origin of cosmic rays
title_fullStr Particle spectra and mass composition in the ultra-high energy region in the framework of the Galactic origin of cosmic rays
title_full_unstemmed Particle spectra and mass composition in the ultra-high energy region in the framework of the Galactic origin of cosmic rays
title_short Particle spectra and mass composition in the ultra-high energy region in the framework of the Galactic origin of cosmic rays
title_sort particle spectra and mass composition in the ultra high energy region in the framework of the galactic origin of cosmic rays
url https://doi.org/10.1051/epjconf/201714506004
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