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

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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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Presentation Transcript
slide1

The propagation

of Ultra High Energy CosmicRays in theGalactic magnetic fields

A.Elyiv

B.Hnatyk

Astronomical Observatory of Kyiv National

University, Kyiv, Ukraine

slide2

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.
slide5

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

slide7

Motion of CosmicRays in the Milky Way

1017Ev

1020 Ev

1019 Ev

5·1017 Ev

1018 Ev

slide8

The deviation mapof cosmic rays with energy 1019 eV

in the unpaired magneticfield

Deviation in degree

slide9

The deviation mapof cosmic rays with energy4·1019 eV

in the unpaired magnetic field

Deviation in degree

slide10

The deviation mapof cosmic rays with energy 1020 eV

in the unpaired magnetic field

Deviation in degree

slide11

The deviation mapof cosmic rays with energy 1019 eV

in the paired magnetic field

Deviation in degree

slide12

The deviation mapof cosmic rays with energy4·1019 eV

in the paired magnetic field

Deviation in degree

slide13

The deviation mapof cosmic rays with energy 1020 eV

in the paired magnetic field

Deviation in degree

slide15

Distribution of cosmic rays with energy 1020 eV

after passing the unpaired magnetic field

slide16

Distribution of cosmic rays with energy4·1019 eV

after passing the unpaired magnetic field

slide17

Distribution of cosmic rays with energy 1019 eV

after passing the unpaired magnetic field

slide18

Distribution of cosmic rays with energy 1020 eV

after passing the paired magnetic field

slide19

Distribution of cosmic rays with energy4·1019 eV

after passing the paired magnetic field

slide20

Distribution of cosmic rays with energy 1019 eV

after passing the paired magnetic field

slide21

Connection between the energy of cosmic rays

and module of galactic latitude

Module of galactic latitude

Energy,

eV

slide22

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.