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    Measurement of the Cosmic Ray Helium Energy Spectrum from 70 GeV to 80 TeV with the DAMPE Space Mission
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    Abstract:
    The measurement of the energy spectrum of cosmic ray helium nuclei from 70 GeV to 80 TeV using 4.5 years of data recorded by the Dark Matter Particle Explorer (DAMPE) is reported in this work. A hardening of the spectrum is observed at an energy of about 1.3 TeV, similar to previous observations. In addition, a spectral softening at about 34 TeV is revealed for the first time with large statistics and well controlled systematic uncertainties, with an overall significance of 4.3σ. The DAMPE spectral measurements of both cosmic protons and helium nuclei suggest a particle charge dependent softening energy, although with current uncertainties a dependence on the number of nucleons cannot be ruled out.Received 5 January 2021Revised 25 March 2021Accepted 6 April 2021DOI:https://doi.org/10.1103/PhysRevLett.126.201102© 2021 American Physical SocietyPhysics Subject Headings (PhySH)Research AreasCosmic ray & astroparticle detectorsCosmic ray composition & spectraParticle astrophysicsGravitation, Cosmology & Astrophysics
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    Energy spectrum
    This review focuses on high-energy cosmic rays in the PeV energy range and above. Of particular interest is the knee of the spectrum around 3 PeV and the transition from cosmic rays of Galactic origin to particles from extra-galactic sources. Our goal is to establish a baseline spectrum from 10^14 to 10^20 eV by combining the results of many measurements at different energies. In combination with measurements of the nuclear composition of the primaries, the shape of the energy spectrum places constraints on the number and spectra of sources that may contribute to the observed spectrum.
    Energy spectrum
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    The energy spectrum of ultra-high energy cosmic rays (UHECR) is usually calculated for sources with identical properties. Assuming that all sources can accelerate UHECR protons to the same extremely high maximal energy E_max > 1020 eV and have the steeply falling injection spectrum 1/E2.7, one can reproduce the measured cosmic ray flux above E > 1018 eV. We show that relaxing the assumption of identical sources and using a power-law distribution of their maximal energy allows one to explain the observed UHECR spectrum with the injection 1/E2 predicted by Fermi shock acceleration. We study possible ways to distinguish between these two cases with future experiments.
    Energy spectrum
    Fermi acceleration
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    This review focuses on high-energy cosmic rays in the PeV energy range and above. Of particular interest is the knee of the spectrum around 3 PeV and the transition from cosmic rays of Galactic origin to particles from extra-galactic sources. Our goal is to establish a baseline spectrum from 10^14 to 10^20 eV by combining the results of many measurements at different energies. In combination with measurements of the nuclear composition of the primaries, the shape of the energy spectrum places constraints on the number and spectra of sources that may contribute to the observed spectrum.
    Energy spectrum
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    The paper presents cosmic ray spectrum by Small Cherenkov Yakutsk array data for 20 continuous years of observation. The spectrum is obtained from Cherenkov light flux - the energy scattered by charged particles of air showers in the atmosphere. It has been shown by measurements that in the cosmic ray spectrum there is a break in the slope at energy $ \sim $10$ ^{17} $ eV. The reliability of the result is based on spectra of other compact array experiments and simulations to check for systematic uncertainties, which could affect the shape of the spectrum. Another confirmation is change in mass composition of cosmic ray obtained from longitudinal development of air showers in energy region 10$ ^{16} $-10$ ^{18} $ eV.
    Energy spectrum
    Cherenkov detector
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