Il Nuovo Cimento C

, Volume 12, Issue 4, pp 467–477 | Cite as

Neutron flux generated by cosmic-ray mouns at 5200 hg/cm2 s.r. underground. Depth-neutron intensity curve

  • M. Aglietta
  • G. Badino
  • G. Bologna
  • C. Castagnoli
  • A. Castellina
  • W. Fulgione
  • P. Galeotti
  • O. Saavedra
  • G. Trinchero
  • S. Vernetto
  • V. L. Dadykin
  • F. F. Khalchukov
  • V. B. Kortchaguin
  • P. V. Kortchaguin
  • V. A. Kudryavtsev
  • A. S. Malguin
  • V. G. Ryasny
  • O. G. Ryazhskaya
  • V. F. Yakushev
  • G. T. Zatsepin
Article

Summary

Neutrons induced by cosmic-ray muons are an important source of background for the new, huge underground detectors. Their characteristics (multiplicity and time distribution) are investigated by using the data recorded from December 1985 to February 1988 in the 90 tons liquid scintillator LSD detector of the Mont Blanc Laboratory. The experimental results on the mean number of neutrons produced by a muon per g/cm2, being <E u >=385 GeV, are found to be in good agreement with an expected distribution given by the theoretical power law <N n>=<E μ>0.75.

PACS 94.40

Cosmics rays 

Riassunto

I neutroni indotti dai muoni dei raggi cosmici sono un'importante sorgente di fondo per i nuovi, grandi rivelatori sottoroccia. Le loro caratteristiche (molteplicità e distribuzione temporale) vengono studiate utilizzando i dati registrati tra dicembre 1985 e febbraio 1988 nel rivelatore LSD del Monte Bianco. I risultati sperimentali sul numero medio di neutroni prodotti da un muone per g/cm2, ad <E μ>=385 GeV risultano essere in buon accordo con la distribuzione attesa, descritta dalla legge di potenza <N n>=<E μ>0.75.

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Copyright information

© Società Italiana di Fisica 1989

Authors and Affiliations

  • M. Aglietta
    • 1
    • 2
  • G. Badino
    • 1
    • 2
  • G. Bologna
    • 1
    • 2
  • C. Castagnoli
    • 1
    • 2
  • A. Castellina
    • 1
    • 2
  • W. Fulgione
    • 1
    • 2
  • P. Galeotti
    • 1
    • 2
  • O. Saavedra
    • 1
    • 2
  • G. Trinchero
    • 1
    • 2
  • S. Vernetto
    • 1
    • 2
  • V. L. Dadykin
    • 3
  • F. F. Khalchukov
    • 3
  • V. B. Kortchaguin
    • 3
  • P. V. Kortchaguin
    • 3
  • V. A. Kudryavtsev
    • 3
  • A. S. Malguin
    • 3
  • V. G. Ryasny
    • 3
  • O. G. Ryazhskaya
    • 3
  • V. F. Yakushev
    • 3
  • G. T. Zatsepin
    • 3
  1. 1.Istituto di Cosmogeofisica del C.N.R.Torino
  2. 2.Istituto di Fisica Generale dell'UniversitàTorino
  3. 3.Institute for Nuclear Research of the Academy of Sciences of USSRMoscow

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