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Lateral distribution of the cosmic ray air showers

Lateral distribution of the cosmic ray air showers. Atmospheric muons. Li Huadong(UCAS) Liu Gang(Tsinghua) Wu Ze(NCEPU). Outline. 1. Background and motivation 2. Detection approaches and techniques 3. Measurement of muon flux and data analysis

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Lateral distribution of the cosmic ray air showers

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  1. Lateral distribution of the cosmic ray air showers Atmospheric muons Li Huadong(UCAS) Liu Gang(Tsinghua) Wu Ze(NCEPU)

  2. Outline 1. Background and motivation 2. Detection approaches and techniques 3. Measurement of muon flux and data analysis 4. Lateral distribution of muon flux and data analysis 5. Summary and outlook

  3. Background and motivation 1. Cosmic rays(99% nuclei, 1% electrons, photons) outside the solar system produce showers of particles when they enter Earth's atmosphere and interactions with ari nuclei occur subsequently. 2. Lateral distribution of rays refers to the laterally spread particles which acquire transverse momentum. 3. The dominant channels for originating muons are secondary charged pions and kaons.

  4. Background and motivation We want to: 1) explore the origin and role of cosmic rays. 2) have a better understand of the universe. 3) go home and not to be cooked, eaten by students who will participate in here next year.

  5. Detection approachs 1. Direct detection: stratospheric ballons, satellites(AMS-02). 2. Indirect detection: detectors on ground(air shower)

  6. Detection techniques on air shower 1. Shower Longitudinal Profile: Fluorescence detection. 2. Lateral Distribution of Particles: Water Cherenkov stations, Scintillators(Muon detector, e/γ detector).

  7. Fluorescence detection Water Cherenkov stations

  8. Measurement of muon flux Wu Ze(NCEPU)

  9. Muon detectors plastic scintillator

  10. Efficiency of PS E1=PM123/（PM3*PM2) E2=PM123/（PM3*PM1) E3=PM123/（PM1*PM2)

  11. Solid angle Two cases: 1.Use the rectangle directly 2.Tranfer the area of rectangle to circle The No.2 is more precise

  12. Data analysis Flux=N123/(E1*E2*E3*S*Ω*T)

  13. Lateral distribution atmospheric muons Liu Gang(Tsinghua)

  14. Lateral distribution atmospheric muons d Muon flux

  15. d Results after we take into account the efficiencies of detectors'

  16. Measurement of lateral muons Counts of muon numbers

  17. Lateral distribution and data analysis Number density of muon flux: 1.795±0.019/s

  18. Summary and outlook . Detection on muon flux is a promsing area of astroparticle physics . Experiments on cosmic rays require much long time to carry on and we should be patient and attentive . We can have a better understaning of the universe, and we will have a better understaning of the universe!

  19. There is still a long way to go... Merci!

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