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Sources of Cosmic Rays

This article discusses the Yakutsk Extensive Air Shower Array and its purpose in investigating the properties of cosmic rays, such as energy spectrum, composition, and anisotropy. It also explores the sources of cosmic rays and the need for confirmations in the field of astrophysics.

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Sources of Cosmic Rays

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  1. Sources of Cosmic Rays E.G.Berezhko Yu.G.Shafer Institute of Cosmophysical Research and Aeronomy Yakutsk, Russia • CR astrophysics with Yakutsk Extensive Air Shower (EAS) array • Determination of CRs sources with gamma-ray telescopes • Conclusions

  2. Yakutsk

  3. Cosmic Rays V.Hess (1912) I ≈ 1 particle/(cm2s) CR origin problem: i) CR source (?) ii) Acceleration mechanism (?) Earth Atmosphere

  4. Cosmic Ray Flux CR sources: Confirmations are still needed Galactic SNRs knee Galactic SNRs Transition from Galactic to Extragalactic CRs ankle Extragalactic (AGNs ?) end of CR spectrum (GZK cutoff?)

  5. Yakutsk Extensive Air Shower Array • Operates since 1973 • Designed for registration of Extensive Air Showers of secondary • particles, produced by high energy Cosmic Ray particle • in the Earth atmosphere • Includes electron, muon and Cherenkov light detectors • Purpose: Investigation of Cosmic Rays properties – energy spectrum, • composition, anisotropy – within the energy range 1015-1020 eV • in order to determine CR sources

  6. Registration stations Yakutsk EASA

  7. Extensive Air Shower (EAS) Yakutsk EAS Array (area S=12 km2) Single array station - Surface detectors (49x2+10) - Cherenkov light detectors (32) - Muon detectors S=20 m2 (5) - Large muon detector S=180 m2 - Differential detectors of Cherenkovlight (2) - Future differential detector

  8. Ykutsk EAS array includes: • 49 basic stations on 12 km2 area, • equipped with two 2 m2 scintillation detectors and • with Cherenkov light detector • 5 muon detectors of 20 m2 (1 GeV threshold) • 2 differential Cherenkov detectors • Muon detector of 180 m2 • 10 additional scintillation detectors • and 14 Cherenkov detectors within the central part • for registration of EAS with energies 1014-1017 eV

  9. Modernization of Yakutsk EAS array Supplement by new detectors: differential Cherenkov light detectors to study Cosmic Ray composition Detector synchronization will be improved from 100 ns up to 10 ns Better angular resolution: Old New

  10. Wide Field Of View Cherenkov telescope Multianode PMT, (Hamamatsu R2486, 16x16 wires anode) Spherical mirror, D=26 cm, F=13 cm Mission: detection of the angular and temporal profile of Cherenkov light induced by EAS at energies ε>1015 eV, in order to study mass composition of CRs

  11. Cosmic Ray spectrum and composition Precise measurement of CR spectrum and composition at 1017-1019 eV is needed to find transition region between galactic and extragalactic CR components Extragalactic CRs CRs from Galactic SuperNova Remnants SN Ia + extragalactic CRs Galactic CRs Galactic CRs (from SNRs SN Ia + SN IIb) + extragalactic CRs Galactic CRs Transition from Galactic to Extragalactic CR component Extragalactic CRs

  12. Main nonthermal emission produced by Cosmic Rays(how one can “see” CR sources) • Synchrotron radiation radio B X-ray e • Inverse Compton scattering  gamma-rays  e  Detection of high-energy gamma-rays provide information about the sources of hadronic CR component • Nuclear collisions  N gamma-rays p

  13. H.E.S.S. Cherenkov telescopes – instruments for detection of TeV-emission MAGIC VERITAS (photomontage)

  14. Institutes achievements • CR transport equation (1964) • Diffusive shock acceleration process (1977) • Nonlinear kinetic theory for CR acceleration in SNRs (1993) • Detailed predictions of expected nonthermal emission, • produced by CRs in SNRs G.F. Krymsky

  15. Energy spectra of SNR nonthermal emission SNR RXJ1713.3-3946 SNR SN 1006 Fermi LAT SNR RX0862.0-4622 Tycho’s SNR

  16. Conclusions • Existing data are consistent with SNRs as the main source • of CRs with energies ε < 1017 eV • Transition energy region from Galactic to Extragalactic CR components • is not determined yet, since the existing estimates • of CR composition are rather contradictory • The progress in resolving of CR origin problem will be achieved • on the basis of new generation • of ground based instruments (Cherenkov telescopes and EASAs) • as well as space gamma-ray telescopes with better characteristics

  17. Spatially integrated energy spectrum of nonthermal emission of SN 1006 Berezhko, Ksenofontov, Völk (2012) NE rim SW rim

  18. Energy spectrum of nonthermal emission of RXJ1713 Berezhko & Völk (2006) SN II/Ib age T ≈ 1600 yr distance d ≈ 1 kpc

  19. Energy spectrum of nonthermal emission of RXJ0852.0-4622 Theory: Berezhko et al. (2006) ExperimentHESS: Aharonian et al. (2005) Fermi: Tanaka et al. (2011) Fermi LAT

  20. Energy spectrum of nonthermal emission of Tycho’s SNR Теория:Berezhko et al. (2002) Эксперимент SHALON:Sinitsina et al. (2003) В = 300 мкГс

  21. Energy spectrum of nonthermal emission of Tycho’s SNR

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