Fine structure of all-particle energy spectrum in the knee region

Garyaka, A. P.; Мартиросов, Р. М.; Ter–Antonyan, S.; Babayan, H. A.; Erlykin, A.D.; Gallant, Y. A.; Jones, L. W.; Kempa, J.; Nikolskaya, N. M.; Pattison, B.; Procureur, J.; Sokhoyan, S. H.; Vardanyan, H.

doi:10.1088/1742-6596/409/1/012081

Cited by 3 publications

(6 citation statements)

References 11 publications

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“…2 for standardized shower size spectra from Fig. 1 in the whole measurement range and near-vertical shower muon truncated size spectra detected by the GAMMA array [20,28]. The results are presented in Fig.…”

Section: Multi-population Dsa Spectral Modelmentioning

confidence: 96%

“…This approach, the so called parametrized regularization of the inverse problem, was implemented in [25] (U ≡ N e ) for AKENO [26] data, in [27] for MAKET-ANI data (U ≡ (N ch , θ)) and in [12] for GAMMA array data (U ≡ (N ch , N µ , cosθ, s)). The application of this regularization method for GAMMA array data (U ≡ (N ch , N µ , cosθ)) [28] and different primary spectral models are presented in Section IV.…”

Section: Inverse Problemmentioning

confidence: 99%

“…The reconstructions of energy spectra in the knee region for A ≡ H, He primary nuclei and A ≡ O-like and F e-like nuclei species were carried out on the basis of standardized shower spectra from Fig. 1 and nearvertical (sec θ < 1.2) shower muon truncated (r µ < 100 m) size spectra measured by the GAMMA array [20,28] for 2003-2010. The kernel functions K A (E|N ch , N µ , θ) for BASJE-MAS, Tibet, GAMMA and KASCADE arrays were simulated by the CORSIKA code [29] in the frames of SIBYLL [31] interaction model for A ≡ H, He, O and F e primary nuclei.…”

Section: A Kernel Functionsmentioning

confidence: 99%

“…The results of the overall shower size spectrum and the truncated muon size spectrum of GAMMA array [20,28] are presented in Fig. 4 along with expected responses according to the Sharp Knee energy spectra (hollow symbols).…”

Section: Figmentioning

confidence: 99%

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Sharp knee phenomenon of primary cosmic ray energy spectrum

Ter–Antonyan¹

2014

Phys. Rev. D

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Primary energy spectral models are tested in the energy range of 1 − 200 PeV using standardized extensive air shower responses from BASJE-MAS, Tibet, GAMMA and KASCADE scintillation shower arrays. Results point towards the two-component origin of observed cosmic ray energy spectra in the knee region (GAPS spectral model) consisting of a pulsar component superimposed upon rigidity-dependent power law diffuse galactic flux. The two-component energy spectral model accounts for both the sharp knee shower spectral phenomenon and observed irregularity of allparticle energy spectrum in the region of 50 − 100 PeV. Alternatively, tested multi-population primary energy spectra predicted by non-linear diffusive shock acceleration (DSA) models describe observed shower spectra in the knee region provided that the cutoff magnetic rigidities of accelerating particles are 6±0.3 PV and 45±2 PV for the first two populations respectively. Both tested spectral models confirm the predominant H − He primary nuclei origin of observed shower spectral knee. The parameters of tested energy spectra are evaluated using solutions of inverse problem on the basis of the corresponding parameterizations of energy spectra for primary H, He, O-like and F elike nuclei, standardized shower size spectral responses in the 550 − 1085 g/cm 2 atmospheric slant depth range and near vertical muon truncated size spectra detected by the GAMMA array.

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Section: Multi-population Dsa Spectral Modelmentioning

confidence: 96%

Section: Inverse Problemmentioning

confidence: 99%

Section: A Kernel Functionsmentioning

confidence: 99%

Section: Figmentioning

confidence: 99%

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Sharp knee phenomenon of primary cosmic ray energy spectrum

Ter–Antonyan¹

2014

Phys. Rev. D

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“…The primary electron-to-proton ratio at relativistic energies is set by the normalization factor K ep = 0.03 (e.g., Park et al, 2015). Figure 2: All-particle energy spectrum: data points from Tunka-25, KASCADE-Grande, Tibet-III, GAMMA, Tunka-133 and IceTop-73 (Aartsen et al, 2013;Amenomori et al, 2008;Apel et al, 2009;Berezhnev et al, 2012b;Budnev et al, 2013;Garyaka et al, 2013) along with the calculated all-particle CR flux from a 3000 year old CSF source (black lines) and from a 10 4 year old CSF source (dashed gray lines) for the distances from the Earth as indicated.…”

Section: The Contribution Of Supernovae In Stellar Clusters To the Crmentioning

confidence: 99%

Supernovae in compact star clusters as sources of high-energy cosmic rays and neutrinos

Bykov

Ellison

Gladilin

et al. 2018

Advances in Space Research

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We discuss a specific population of galactic PeVatrons which may be the main source of the galactic (cosmic-ray) (CR) component well above PeV energies. Supernovae in compact clusters of massive stars are proposed as powerful sources of CRs, neutrinos, and γ-ray emission. Numerical simulations of non-linear Fermi acceleration at converging shock flows have revealed that these accelerators can provide very hard spectra of protons up to 10 16 − 10 17 eV which is well above the "knee" in the all-particle CR spectrum at about 3 × 10 15 eV. We suggest that known supernova remnants interacting with stellar winds in the compact clusters of young massive stars Westerlund I and Cl*1806-20 can be associated with the sources of the TeV γ-ray emission detected by H.E.S.S. and may be responsible for a fraction of the high-energy neutrinos detected with the IceCube observatory. A recent CR composition measurement with the LOFAR array has revealed a light-mass component possibly dominating the all-particle spectrum at energies around 10 17 eV. Such a strong light component (mainly protons and helium) may require specific galactic CR sources such as supernovae interacting with compact clusters of massive stars in addition to isolated supernova remnants.

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Spectrum and anisotropy of cosmic rays at TeV–PeV-energies and contribution of nearby sources

Sveshnikova

Strelnikova

Птускин

2013

Astroparticle Physics

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The role of nearby galactic sources, the supernova remnants, in formation of observed energy spectrum and large-scale anisotropy of high-energy cosmic rays is studied. The list of these sources is made up based on radio, X-ray and gamma-ray catalogues. The distant sources are treated statistically as ensemble of sources with random positions and ages. The source spectra are defined based on the modern theory of cosmic ray acceleration in supernova remnants while the propagation of cosmic rays in the interstellar medium is described in the frameworks of galactic diffusion model. Calculations of dipole component of anisotropy are made to reproduce the experimental procedure of "twodimensional" anisotropy measurements. The energy dependence of particle escape time in the process of acceleration in supernova remnants and the arm structure of sources defining the significant features of anisotropy are also taken into account. The essential new trait of the model is a decreasing number of core collapse SNRs being able to accelerate cosmic rays up to the given energy, that leads to steeper total cosmic ray source spectrum in comparison with the individual source spectrum. We explained simultaneously the new cosmic ray data on the fine structure of all particle spectrum around the knee and the amplitude and direction of the dipole component of anisotropy in the wide energy range 1 TeV1 EeV. Suggested assumptions do not look exotic, and they confirm the modern understanding of cosmic ray origin.

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Fine structure of all-particle energy spectrum in the knee region

Cited by 3 publications

References 11 publications

Sharp knee phenomenon of primary cosmic ray energy spectrum

Sharp knee phenomenon of primary cosmic ray energy spectrum

Supernovae in compact star clusters as sources of high-energy cosmic rays and neutrinos

Spectrum and anisotropy of cosmic rays at TeV–PeV-energies and contribution of nearby sources

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