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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 CosmicRays in theGalactic magnetic fields

A.Elyiv

B.Hnatyk

Astronomical Observatory of Kyiv National

University, Kyiv, Ukraine


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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.



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Arrival Directions of Cosmic Rays


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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



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Motion of CosmicRays in the Milky Way

1017Ev

1020 Ev

1019 Ev

5·1017 Ev

1018 Ev


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The deviation mapof cosmic rays with energy 1019 eV

in the unpaired magneticfield

Deviation in degree


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The deviation mapof cosmic rays with energy4·1019 eV

in the unpaired magnetic field

Deviation in degree


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The deviation mapof cosmic rays with energy 1020 eV

in the unpaired magnetic field

Deviation in degree


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The deviation mapof cosmic rays with energy 1019 eV

in the paired magnetic field

Deviation in degree


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The deviation mapof cosmic rays with energy4·1019 eV

in the paired magnetic field

Deviation in degree


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The deviation mapof cosmic rays with energy 1020 eV

in the paired magnetic field

Deviation in degree



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Distribution of cosmic rays with energy Earth 1020 eV

after passing the unpaired magnetic field


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Distribution of cosmic rays with energy Earth4·1019 eV

after passing the unpaired magnetic field


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Distribution of cosmic rays with energy Earth 1019 eV

after passing the unpaired magnetic field


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Distribution of cosmic rays with energy Earth 1020 eV

after passing the paired magnetic field


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Distribution of cosmic rays with energy Earth4·1019 eV

after passing the paired magnetic field


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Distribution of cosmic rays with energy Earth 1019 eV

after passing the paired magnetic field


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C Earthonnection between the energy of cosmic rays

and module of galactic latitude

Module of galactic latitude

Energy,

eV


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C Earthonclusions

  • 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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