Origin of Galactic Cosmic Rays from Supernova Remnants

Berezhko, E. G.

doi:10.1016/j.nuclphysbps.2014.10.003

Cited by 13 publications

(9 citation statements)

References 103 publications

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“…The mechanism by which cosmic rays are produced and accelerated has been a topic of extensive interest. For galaxies, supernovae remnants (SNR) are considered to be the main sources of cosmic rays [41][42][43][44][45]. While SNRs are thought to provide the dominant contribution of cosmic rays in galaxies, other mechanisms such as pulsars and their nebula can also provide significant contributions to the total cosmic ray population [46][47][48].…”

Section: Introductionmentioning

confidence: 99%

Exploring a cosmic-ray origin of the multiwavelength emission in M31

2019

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A recent detection of spatially extended gamma-ray emission in the central region of the Andromeda galaxy (M31) has led to several possible explanations being put forth, including dark matter annihilation and millisecond pulsars. Another possibility is that the emission in M31 can be accounted for with a purely astrophysical cosmic-ray (CR) scenario. This scenario would lead to a rich multi-wavelength emission that can, in turn, be used to test it. Relativistic cosmic-ray electrons (CRe) in magnetic fields produce radio emission through synchrotron radiation, while X-rays and gamma rays are produced through inverse Compton scattering. Additionally, collisions of primary cosmic-ray protons (CRp) in the interstellar medium produce charged and neutral pions that then decay into secondary CRe (detectable through radiative processes) and gamma-rays. Here, we explore the viability of a CR origin for multi-wavelength emission in M31, taking into consideration three scenarios: a CR scenario dominated by primary CRe, one dominated by CRp and the resulting secondary CRe and gamma rays from neutral pion decay, and a final case in which both of these components exist simultaneously. We find that the multi-component model is the most promising, and is able to fit the multi-wavelength spectrum for a variety of astrophysical parameters consistent with previous studies of M31 and of cosmic-ray physics. However, the CR power injection implied by our models exceeds the estimated CR power injection from typical astrophysical cosmic-ray sources such as supernovae.

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Section: Introductionmentioning

confidence: 99%

Exploring a cosmic-ray origin of the multiwavelength emission in M31

2019

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“…Berezhko & Völk 2000). The application of this theory to individual SNRs (see Völk 2004;Berezhko 2005Berezhko , 2008Berezhko , 2014, for reviews) has demonstrated its ability to explain the observed SNR properties and radiation spectra. Combining the theoretical model with the observed synchrotron spectra predicts new effects like the large degree of magnetic field amplification that leads to the observed concentration of the highest-energy electrons in a very thin shell just behind the forward shock into the circumstellar medium (CSM).…”

Section: Introductionmentioning

confidence: 99%

Re-Examination of the Expected Gamma-Ray Emission of Supernova Remnant Sn 1987a

Berezhko

Ksenofontov

Völk

2015

ApJ

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A nonlinear kinetic theory, combining cosmic-ray (CR) acceleration in supernova remnants (SNRs) with their gas dynamics, is used to re-examine the nonthermal properties of the remnant of SN 1987A for an extended evolutionary period of 5-50 yr. This spherically symmetric model is approximately applied to the different features of the SNR which consist of (i) a blue supergiant wind and bubble, and (ii) of the swept-up red supergiant (RSG) wind structures in the form of an H II region, an equatorial ring (ER), and an hourglass region. The RSG wind involves a mass loss rate that decreases significantly with elevation above and below the equatorial plane. The model adapts recent threedimensional hydrodynamical simulations by Potter et al. in 2014 that use a significantly smaller ionized mass of the ER than assumed in the earlier studies by the present authors. The SNR shock recently swept up the ER, which is the densest region in the immediate circumstellar environment. Therefore, the expected gamma-ray energy flux density at TeV energies in the current epoch has already reached its maximal value of ∼ 10 −13 erg cm −2 s −1 . This flux should decrease by a factor of about two over the next 10 years. Subject headings: acceleration of particles -ISM: individual objects (SN 1987A) -ISM: supernova remnants -X-rays: individual (SN 1987A) -gamma rays: ISM

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“…We have used approximations (eqn. (1)) for (dI p /dE) and (dI He /dE) based on Berezhko calculations [32] and normalized at AMS-02 data at 1.8 TeV [21]. Figures 1 and 2 demonstrate how these approximations fit the data [21][22][23][24][25][26][27][28][29][30][31].…”

Section: Methodsmentioning

confidence: 99%

“…Indeed, there are results of many measurements of the fluxes of the primary cosmic nuclei (e.g.AMS-02 [21], PAMELA [22], ATIC-2 [23], CREAM [24], ARGO-YBJ [25], ARGO-YBJ & FWCTA [26], KASCADE [27], KASCADE-Grande [28], Tunka [29], IceCube [30], Telescope Array [31]). Besides there are some calculations of spectra of the primary proton and helium nuclei in SNR [32]. We will use these ap-EPJ Web of Conferences 208, (2019) https://doi.org/10.1051/epjconf/201920807004 ISVHECRI 2018 Figure 1.…”

Section: Introductionmentioning

confidence: 99%

Testing of almost all the hadronic interaction models by comparing calculated muon energy spectrum with data

et al. 2019

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Uncertainties of the model energy spectra of the most energetic secondary charged mesons are discussed. Computer simulations of the partial energy spectra of the atmospheric vertical muons induced by primary cosmic particles with various fixed energies in terms of hadronic interactions models had been carried out with the help of the CORSIKA package. These partial spectra have been convolved with the contemporary spectra of the primary cosmic particles in the energy range 0.1-10 000 TeV. Results of simulations are compared with the contemporary data of the atmospheric vertical muon flux. Comparison shows that all models underestimate the production of secondary charged π±-mesons (and K±-mesons) by a factor of ~ 1.4 ÷ 2 at the highest energies. This underestimation induces a more rapid development of extensive air showers in the atmosphere and results in uncertainties in estimates of energy and composition of the primary cosmic particles.

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Origin of Galactic Cosmic Rays from Supernova Remnants

Cited by 13 publications

References 103 publications

Exploring a cosmic-ray origin of the multiwavelength emission in M31

Exploring a cosmic-ray origin of the multiwavelength emission in M31

Re-Examination of the Expected Gamma-Ray Emission of Supernova Remnant Sn 1987a

Testing of almost all the hadronic interaction models by comparing calculated muon energy spectrum with data

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