Selected Topics in Cosmic Ray Physics

Aloisio, Roberto; Blasi, Pasquale; Mitri, I. De; Petrera, S.

doi:10.1007/978-3-319-65425-6_1

Cited by 25 publications

(51 citation statements)

References 417 publications

(674 reference statements)

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“…This latter conclusion appears to confirm a tentative trend, based on older experiments as well, to locate the proton knee at somewhat lower energies for experiments at altitude closer to the maximum of the shower induced by CRs in the atmosphere (see Ref. [15] for a recent review). This is also expected to make the dependence of the results on the adopted hadronic model weaker than for experiments at sea level.…”

Section: The Flux Of Primary Crs and The Rigidity Of The Kneesupporting

confidence: 78%

Atmospheric neutrinos and the knee of the cosmic ray spectrum

Mascaretti

Blasi

Evoli

2020

Astroparticle Physics

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The nature of the knee in the all-particle spectrum of cosmic rays remains subject of much investigation, especially in the aftermath of recent measurements claiming the detection of a knee-like feature in the spectrum of the light component of cosmic rays at energy ∼ 700 TeV, at odds with the standard picture in which the knee in the all-particle spectrum is dominated by light cosmic rays. Here we investigate the implications of this and other scenarios in terms of the measured flux of atmospheric neutrinos. In particular we discuss the possibility that the spectrum of atmospheric neutrinos in the region 50 TeV may provide information about the different models for the mass composition in the knee region. We investigate the dependence of the predicted atmospheric neutrino flux on the shape of the light cosmic ray spectra and on the interaction models describing the development of showers in the atmosphere. The implications of all these factors for the identification of the onset of an astrophysical neutrino component are discussed.

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Section: The Flux Of Primary Crs and The Rigidity Of The Kneesupporting

confidence: 78%

Atmospheric neutrinos and the knee of the cosmic ray spectrum

Mascaretti

Blasi

Evoli

2020

Astroparticle Physics

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“…which is then used to determine numerically the δ k values in Eq. (11). The normalization of ω is such that E ¼ 2πA 0 Δt R δ 3 δ 0 dδ cos δωðδÞ.…”

Section: Appendix E: Directional Exposure and Expectations From Anisomentioning

confidence: 99%

“…Accurate knowledge of the cosmic-ray flux as a function of energy is required to help discriminate between competing models of cosmic-ray origin. As a result of earlier work with the HiRes instrument [3], the Pierre Auger Observatory [4] and the Telescope Array [5], two spectral features were identified beyond reasonable doubt (see, e.g., [6][7][8][9][10][11] for recent reviews). These are a hardening of the spectrum at about 5 × 10 18 eV (the ankle) and a strong suppression of the flux at an energy about a decade higher.…”

Section: Introductionmentioning

confidence: 99%

Measurement of the cosmic-ray energy spectrum above 2.5×1018 eV using the Pierre Auger Observatory

Aab¹,

Abreu²,

Aglietta³

et al. 2020

Phys. Rev. D

137

107

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We report a measurement of the energy spectrum of cosmic rays for energies above 2.5 × 10 18 eV based on 215,030 events recorded with zenith angles below 60°. A key feature of the work is that the estimates of the energies are independent of assumptions about the unknown hadronic physics or of the primary mass composition. The measurement is the most precise made hitherto with the accumulated exposure being so large that the measurements of the flux are dominated by systematic uncertainties except at energies above 5 × 10 19 eV. The principal conclusions are (1) The flattening of the spectrum near 5 × 10 18 eV, the so-called "ankle," is confirmed. (2) The steepening of the spectrum at around 5 × 10 19 eV is confirmed. (3) A new feature has been identified in the spectrum: in the region above the ankle the spectral index γ of the particle flux (∝ E −γ) changes from 2.51 AE 0.03 ðstatÞ AE 0.05 ðsystÞ to 3.05 AE 0.05 ðstatÞ AE 0.10 ðsystÞ before changing sharply to 5.1 AE 0.3 ðstatÞ AE 0.1 ðsystÞ above 5 × 10 19 eV. (4) No evidence for any dependence of the spectrum on declination has been found other than a mild excess from the Southern Hemisphere that is consistent with the anisotropy observed above 8 × 10 18 eV.

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“…This should be compared with the emissivity in UHECRs. It was shown that the emissivity required to reproduce the UHECR data above 10 18 eV should be of the order 10 45 − 10 46 erg Mpc −3 yr −1 [16] which corresponds to ∼ 10 43 − 10 44 erg Mpc −3 yr −1 above 10 20 eV. Our own calculation which follows the approach of [17] using the photo-pion production cross-section from [18] gave the values of 7.5 × 10 43 erg Mpc −3 yr −1 and 1.2 × 10 43 erg Mpc −3 yr −1 .…”

Section: Methodsmentioning

confidence: 99%

Ultra-high energy cosmic rays and the strongest AGN flares

Пширков

Nizamov

2018

EPJ Web Conf.

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We perform an observational test of the hypothesis that ultra-high energy cosmic rays (E > 1020 eV) are accelerated in giant flares of active galactic nuclei (AGN). We use the observations of Fermi LAT during the first 7.4 years of the mission. We select highly variable AGNs with the redshift z ≤ 0:3 and use an empirical relation between the bolometric luminosity and the jet kinetic power in order to find the local kinetic emissivity of strong AGN flares: L ~ 1:1 × 1045erg Mpc-3 yr-1. This is approximately one order of magnitude larger than the UHECR emissivity estimated from the data of Pierre Auger and Telescope Array observatories which makes the whole scenarion feasible provided the acceleration spectrum is sufficiently hard and/or narrow.

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Selected Topics in Cosmic Ray Physics

Cited by 25 publications

References 417 publications

Atmospheric neutrinos and the knee of the cosmic ray spectrum

Atmospheric neutrinos and the knee of the cosmic ray spectrum

Measurement of the cosmic-ray energy spectrum above 2.5×1018 eV using the Pierre Auger Observatory

Ultra-high energy cosmic rays and the strongest AGN flares

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