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The propagation of Ultra High Energy Cosmic Rays in the Galactic magnetic fields

The propagation of Ultra High Energy Cosmic Rays in the Galactic magnetic fields A. Elyiv B. Hnatyk Astronomical Observatory of Kyiv National University, Kyiv, Ukraine Content of presentation: Introduction. The problem of Ultra High Energy Cosmic Rays .

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The propagation of Ultra High Energy Cosmic Rays in the Galactic magnetic fields

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  1. The propagation of Ultra High Energy CosmicRays in theGalactic magnetic fields A.Elyiv B.Hnatyk Astronomical Observatory of Kyiv National University, Kyiv, Ukraine

  2. Content of presentation: • Introduction. The problem of Ultra High Energy CosmicRays. • The magnetic field model of Milky Way. • The maps of deviationof cosmic rays in the magnetic field. • Distribution of cosmic raysafter magnetic field of Galaxy. • Connection between the energy of cosmic rays and module of galactic latitude. • Conclusions.

  3. AGASA Energy Spectrum

  4. Arrival Directions of Cosmic Rays

  5. Magnetic field of the Milky Way P.G. Tinyakov, I.I Tkachev. Tracing protons through the galactic magnetic field: a clue for charge composition of ultra-high energy cosmic rays. Astro-ph/0111305 R=8.5 кpс - distance between the Sun and center of the Milky Way B0=1.4 μG - strength of magnetic field near the Sun p=-8o - pitch angle d=-0.5 кpс - distance from the Sun to the first field reversal, negative d means that nearest reversal occurs in the direction to the Galactic center. h=1.5 кpс - a height of the disc The center of Galaxy The Sun paired field - law of motion unpaired field

  6. Magnetic field of the Milky Way μG

  7. Motion of CosmicRays in the Milky Way 1017Ev 1020 Ev 1019 Ev 5·1017 Ev 1018 Ev

  8. The deviation mapof cosmic rays with energy 1019 eV in the unpaired magneticfield Deviation in degree

  9. The deviation mapof cosmic rays with energy4·1019 eV in the unpaired magnetic field Deviation in degree

  10. The deviation mapof cosmic rays with energy 1020 eV in the unpaired magnetic field Deviation in degree

  11. The deviation mapof cosmic rays with energy 1019 eV in the paired magnetic field Deviation in degree

  12. The deviation mapof cosmic rays with energy4·1019 eV in the paired magnetic field Deviation in degree

  13. The deviation mapof cosmic rays with energy 1020 eV in the paired magnetic field Deviation in degree

  14. Initial direction of cosmic rays which have started from the Earth

  15. Distribution of cosmic rays with energy 1020 eV after passing the unpaired magnetic field

  16. Distribution of cosmic rays with energy4·1019 eV after passing the unpaired magnetic field

  17. Distribution of cosmic rays with energy 1019 eV after passing the unpaired magnetic field

  18. Distribution of cosmic rays with energy 1020 eV after passing the paired magnetic field

  19. Distribution of cosmic rays with energy4·1019 eV after passing the paired magnetic field

  20. Distribution of cosmic rays with energy 1019 eV after passing the paired magnetic field

  21. Connection between the energy of cosmic rays and module of galactic latitude Module of galactic latitude Energy, eV

  22. Conclusions • Magnetic field of our Galaxy is (4μG) and alike the extragalactic magnetic field (10-8 G) has considerable influence on propagation of cosmic rays. • For cosmic rays with energies 4·1019eV average declination equals 5º, for 1020 eV only 2º • We discover equatorial zone where cosmic rays are absence. This is the zone of avoidance for CR.So, for energy 1019 еV this zone is equal to 40º. Therefore, the rays in the figure are moved out to side of North galactic pole for paired magnetic field.

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