Cosmic Rays in Galactic and Extragalactic Magnetic Fields

Aharonian, F.; Bykov, A. M.; Parizot, E.; Птускин, В. С.; Watson, Alan

doi:10.1007/s11214-011-9770-3

Cited by 48 publications

(44 citation statements)

References 153 publications

(132 reference statements)

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“…For recent reviews on UHECR observations and related models see [33,34,35]. The discussion above demonstrates the importance of a theoretical study of nuclei as carriers of the UHE signal.…”

Section: Introductionmentioning

confidence: 94%

Analytic calculations of the spectra of ultra-high energy cosmic ray nuclei. I. The case of CMB radiation

Aloisio

Berezinsky

Grigorieva

2013

Astroparticle Physics

124

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We present a systematic study of different methods for the analytic calculation of ultra-high energy nuclei diffuse spectra. Nuclei propagating in the intergalactic space are photo-disintegrated and decrease their Lorentz factor due to the interaction with cosmic microwave background and extragalactic background light. We calculate the evolution trajectories in the backward time, that describe how atomic mass number A and Lorentz factor Γ change with redshift z. Three methods of spectra calculations are investigated and compared: (i) trajectory method, (ii) kinetic equation combined with trajectory calculations and (iii) coupled kinetic equations. We believe that these three methods exhaust at least the principal possibilities for any analytic solution of the problem. In the most straightforward method (i) only trajectory calculations are used to connect the observed nuclei flux with the production rate of primary (accelerated) nuclei A 0 . In the second method (ii) the flux (space density) of primary nuclei, and secondary nuclei and protons are calculated with the help of kinetic equation and trajectories are used only to determine the generation rates of these nuclei. The third method (iii) consists in solving the complete set of coupled kinetic equations, written starting with primary nuclei A 0 , then for A 0 − 1 etc down to the A of interest. The solution of the preceding equation gives the generation rate for the one which follows. An important element of the calculations for all methods is the systematic use of Lorentz factor instead of energy. We consider here the interaction of nuclei only with the cosmic microwave background, this case is particularly suitable for understanding the physical results. In paper (II) of this series the extragalactic background light will be also included. Estimating the uncertainties of all methods discussed above, we conclude that the method of coupled kinetic equations gives the most reliable results.

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Section: Introductionmentioning

confidence: 94%

Analytic calculations of the spectra of ultra-high energy cosmic ray nuclei. I. The case of CMB radiation

Aloisio

Berezinsky

Grigorieva

2013

Astroparticle Physics

124

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“…Cosmic rays are energetic particles propagating within the Galaxy, and are divided into primary and secondary types [27][28][29][30]. Primary cosmic rays are likely to originate from powerful astrophysical processes, such as supernova explosions and pulsars.…”

Section: Injection and Propagation Of Cosmic Raysmentioning

confidence: 99%

AMS-02 fits dark matter

Balázs

2016

J. High Energ. Phys.

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In this work we perform a comprehensive statistical analysis of the AMS-02 electron, positron fluxes and the antiproton-to-proton ratio in the context of a simplified dark matter model. We include known, standard astrophysical sources and a dark matter component in the cosmic ray injection spectra. To predict the AMS-02 observables we use propagation parameters extracted from observed fluxes of heavier nuclei and the low energy part of the AMS-02 data. We assume that the dark matter particle is a Majorana fermion coupling to third generation fermions via a spin-0 mediator, and annihilating to multiple channels at once. The simultaneous presence of various annihilation channels provides the dark matter model with additional flexibility, and this enables us to simultaneously fit all cosmic ray spectra using a simple particle physics model and coherent astrophysical assumptions. Our results indicate that AMS-02 observations are not only consistent with the dark matter hypothesis within the uncertainties, but adding a dark matter contribution improves the fit to the data. Assuming, however, that dark matter is solely responsible for this improvement of the fit, it is difficult to evade the latest CMB limits in this model.

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“…The γ -ray luminosity of each remnant L SN R is chosen in a way that the cosmic rays, produced in the remnant, compensate for the observed galactic cosmic ray energy loss [3,9]. To fully characterize the SNR population we also need to specify their distribution in the Galaxy.…”

Section: Estimate Of the Expected Number Of The Observable Snrsmentioning

confidence: 99%

“…The exact origin of the galactic cosmic rays is not known, although for decades the SNRs were favoured as their sources due to their energy budget and number in the Galaxy [e.g. [2][3][4], although alternative models of the CR production exist [5], related to the acceleration by pulsars and/or pulsar wind nebulae [6] or in the larger scale OB associations [e.g. 7,8].…”

Section: Introductionmentioning

confidence: 99%

Comparison of the expected and observed supernova remnant counts with Fermi/LAT

Vovk

Neronov

Malyshev

2015

EPJ Web of Conferences

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Abstract. SNRs are commonly believed to be the accelerators of the galactic cosmic rays -mainly protonsand are expected to produce γ -rays through the inelastic proton-proton collisions. Fermi/LAT was expected to detect many of those, but only a dozen is listed in the recent Fermi/LAT 2nd Source catalogue. To test whether the observed number of SNRs is in agreement with the above assumption, we use a simplified model of an SNR and calculate the predicted amount of the observable remnants taking into account their distribution in the Galaxy and the sensitivity of Fermi/LAT. We find that the observed number of SNRs agrees with the prediction of our model if we assume a low, 1 cm −3 , number density of the SNR's ambient medium. The result, presented here, suggests, that on average the supernova explosions happen in the under-dense regions, such as bubbles, creating by the winds of the progenitor stars. Under this natural supposition our result finds an agreement with the assumption, that the observed population of supernovae remnants is indeed responsible for the production of the galactic cosmic rays.

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Cosmic Rays in Galactic and Extragalactic Magnetic Fields

Cited by 48 publications

References 153 publications

Analytic calculations of the spectra of ultra-high energy cosmic ray nuclei. I. The case of CMB radiation

Analytic calculations of the spectra of ultra-high energy cosmic ray nuclei. I. The case of CMB radiation

AMS-02 fits dark matter

Comparison of the expected and observed supernova remnant counts with Fermi/LAT

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