Energy Spectra of Cosmic-Ray Protons and Nuclei Measured in the NUCLEON Experiment Using a New Method

Bulatov, V.; Vasiliev, О.; Voronin, A.; Gorbunov, N.; Grebenyuk, V.; Dorokhov, V.; Karmanov, D.; Kovalev, I.; Kudryashov, I.; Kurganov, A.; Merkin, M.; Панов, А. Д.; Podorozhny, D.; Polkov, D.; Porokhovoi, S.Yu.; Свешникова, Л.; Ткачев, Л.; Tkachenko, A.; Turundaevskiy, A.; Filippov, S.; Shumikhin, V.

doi:10.1134/s1063772919010013

Cited by 34 publications

(41 citation statements)

References 27 publications

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“…It is also interesting to note that the HAWC measurement of the all-particle spectrum [23] in the 10-500 TeV energy range shows a spectral break at the energy 45.7 ± 0.1 TeV where the index is oberved to change from 2.49 ± 0.01 to 2.71 ± 0.01 (with a step of approximately the same size as the one observed for the proton flux). Evidence for a strong break in the all-particle spectrum at a rigidity 7-17 TV has also been reported by the NUCLEON experiment [8,9].…”

Section: Discussionsupporting

confidence: 64%

“…The existing measurements of helium and other nuclei at E 10 TeV [6,8,9] suggest that the softening is also present for cosmic ray particles heavier than protons, and within the large statistical and systematic errors, the feature is again consistent with having a rigidity dependent shape, common to all particle types. More data are however required to reach a firm conclusion.…”

Section: Discussionmentioning

confidence: 62%

“…The spectral hardening for protons measured by AMS02 is centered at higher rigidity (ρ p 336 +95 −52 GV) in comparison to the PAMELA results, and has a smaller step in spectral index ∆α 0.133 +0.056 −0.037 (with α 1 2.849 +0.006 −0.005 , and α 2 2.716 +0.037 −0.056 ). Measurements of the proton spectrum above 1 TeV have been now obtained by several CR calorimeters: ATIC [5], CREAM [6], CALET [7], NUCLEON [8,9] and DAMPE [10]. The ATIC, CREAM and NUCLEON detectors cover only the energy range E 1 TeV, and therefore do not observe directly the hardening, but only the spectral shape above it.…”

Section: Measurements Of the Cr Proton Spectrummentioning

confidence: 99%

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The shape of the cosmic ray proton spectrum

Lipari

Vernetto

2020

Astroparticle Physics

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Recent observations of cosmic ray protons in the energy range 10 2 -10 5 GeV have revealed that the spectrum cannot be described by a simple power law. A hardening of the spectrum around an energy of order few hundred GeV, first observed by the magnetic spectrometers PAMELA and AMS02, has now been confirmed by several calorimeter detectors (ATIC, CREAM, CALET, NUCLEON and DAMPE). These new measurements reach higher energy and indicate that the hardening corresponds to a larger step in spectral index than what estimated by the magnetic spectrometers. Data at still higher energy (by CREAM, NUCLEON and DAMPE) show that the proton spectrum undergoes a marked softening at E ≈ 10 4 GeV. Understanding the origin of these unexpected spectral features is a significant challenge for models of the Galactic cosmic rays. An important open question is whether additional features are present in the proton spectrum between the softening and the "Knee". Extensive Air Shower detectors, using unfolding procedures that require the modeling of cosmic ray showers in the atmosphere, estimated the proton flux below and around the Knee (at E 3 PeV). These results however have large systematic uncertainties and are in poor agreement with each other. The measurement in the PeV energy range, recently presented by IceTop/IceCube, indicates a proton flux higher than extrapolations of the direct measurements calculated assuming a constant slope, and therefore requires the existence of an additional spectral hardening below the Knee. A clarification of this point is very important for an understanding of the origin of the Galactic cosmic rays, and is also essential for a precise calculation of the spectra of atmospheric neutrinos in the energy range (E 10 TeV) where they constitute the foreground for the emerging astrophysical ν signal.

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Section: Discussionsupporting

confidence: 64%

Section: Discussionmentioning

confidence: 62%

Section: Measurements Of the Cr Proton Spectrummentioning

confidence: 99%

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The shape of the cosmic ray proton spectrum

Lipari

Vernetto

2020

Astroparticle Physics

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“…The absence of structures indicates that a common acceleration mechanism in CR sources is at work and that features connected to the age or maximal energy of individual sources are averaged out, because a large number of sources contributes to the locally observed CR flux. In other words, a AMS-02 CREAM NUCLEON Figure 10: The spectrum of proton, helium and carbon as function of rigidity, measured by the AMS-02 [126,177], CREAM [178] and NUCLEON experiments [179,180].…”

Section: Primary Cosmic Ray Nucleimentioning

confidence: 99%

Cosmic ray models

Kachelrieß

Semikoz

2019

Progress in Particle and Nuclear Physics

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We review progress in high-energy cosmic ray physics focusing on recent experimental results and models developed for their interpretation. Emphasis is put on the propagation of charged cosmic rays, covering the whole range from ∼ (20 − 50) GV, i.e. the rigidity when solar modulations can be neglected, up to the highest energies observed. We discuss models aiming to explain the anomalies in Galactic cosmic rays, the knee, and the transition from Galactic to extragalactic cosmic rays.

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“…Cosmic ray composition studies with HAWC J.C. Arteaga-Velazquez [23], DAMPE [24,25], NUCLEON [26], ARGO-YBJ [27] and MUBEE [28]. over the scenario with only one break in case of the spectra for H, He and H+He.…”

Section: Pos(icrc2021)374mentioning

confidence: 99%

HAWC measurements of the energy spectra of cosmic ray protons, helium and heavy nuclei in the TeV range

Hawc¹,

Abeysekara²,

Albert³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

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Current knowledge of the relative abundances and the energy spectra of the elemental mass groups of cosmic rays in the 10 TeV − 1 PeV interval is uncertain. This situation prevents carrying out precision tests that may lead to distinguish among the existing hypotheses on the origin and propagation of TeV cosmic rays in the galaxy. In order to learn more about the mass composition of these particles, we have employed HAWC data from hadron induced air showers in order to determine the spectra of three mass groups of cosmic rays: protons, helium and heavy nuclei with > 2. The energy spectra were estimated by using the Gold unfolding technique on the 2D distribution of the lateral shower age against the estimated primary energy of events with arrival zenith angles smaller than 45 degrees. The study was carried out based on simulations using the QGSJET-II-04 model. Results are presented for primary cosmic-ray energies from 10 TeV to 251 TeV. They reveal that the aforementioned cosmic ray spectra exhibit fine structures within the above primary energy range.

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Energy Spectra of Cosmic-Ray Protons and Nuclei Measured in the NUCLEON Experiment Using a New Method

Cited by 34 publications

References 27 publications

The shape of the cosmic ray proton spectrum

The shape of the cosmic ray proton spectrum

Cosmic ray models

HAWC measurements of the energy spectra of cosmic ray protons, helium and heavy nuclei in the TeV range

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