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Il Nuovo Cimento B (1965-1970)

, Volume 51, Issue 2, pp 475–482 | Cite as

On the K/π ratio from muonic intensity at 90 m w.e. and at large zenith angles

  • L. Briatore
  • M. Dardo
Article

Summary

We made the measure of cosmic-ray muonic intensity underground at 90 m w.e. and at large zenith angles. The comparison of the experimental data with the directional intensity calculated on the basis of the isobaric-model energy spectra allows us to derive the K/π ratio at production. We obtained K/π≃0.18 in the primary energy interval (∼4·102÷∼104) GeV, in agreement with works of other authors carried out with many different experimental techniques.

Keywords

Zenith Angle Production Spectrum Directional Intensity Muonic Flux Large Zenith Angle 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Об отнощении K/π иэ иэмерения мюонной интенсивности при 90 m w.e. и больщих эенитных углах

Реэюме

Мы провели иэмерение мюонной интенсивности космических лучей под эемлей при 90 m w.e. и больщих эенитных углах. Сравнение зкспериментальных данных с направленной интенсивностью, вычисленной на основе знергетических спектров иэобарической модели, поэволяет нам определить отнощение K/π при рождении. Мы получили K/π=0.18 в интервале первичных знергий∼(4·102÷104) ГзВ, что согласуется с работами других авторов, выполненных с испольэованием раэличных зкспериментальных методик.

Riassunto

Abbiamo effettuato la misura dell’intensità muonica della radiazione cosmica sotto terra a 90 m a.e. e a grandi angoli zenitali. Il confronto dei risultati sperimentali con l’intensità direzionale calcolata in base agli spettri energetici dati dal modello isobarico, ci permette di risalire al rapporto K/π alla produzione. Si ottiene K/π≃0.18 per energie dei primari nell’intervallo (∼4·102÷∼104) GeV, in accordo con lavori di altri autori condotti con tecniche sperimentali diverse.

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References

  1. (1).
    G. Cini Castagnoli andM. A. Dodero:La ricerca scientifica, in press.Google Scholar
  2. (2).
    W. R. Sheldon andN. M. Duller:Nuovo Cimento,23, 63 (1962).CrossRefGoogle Scholar
  3. (3).
    J. E. Allen andA. J. Apostolakis:Proc. Roy. Soc.,265, 117 (1961).ADSCrossRefGoogle Scholar
  4. (4).
    D. Jakeman:Canad. Journ. Phys.,34, 432 (1956).ADSCrossRefGoogle Scholar
  5. (5).
    W. Pak, S. Ozaki, B. P. Roe andK. Greisen:Phys. Rev.,121, 905 (1961).ADSCrossRefGoogle Scholar
  6. (6).
    E. Amaldi, C. Castagnoli, A. Gigli andS. Sciuti:Nuovo Cimento,9, 969 (1952).CrossRefGoogle Scholar
  7. (7).
    D. Tidman andK. Ogilvie:Nuovo Cimento,6, 735 (1957).CrossRefGoogle Scholar
  8. (8).
    K. Maeda:Journ. Atm. Terr. Phys.,19, 184 (1960).ADSCrossRefGoogle Scholar
  9. (9).
    Y. Pal andB. Peters:Mat. Fys. Medd. Dan.,33, n. 15 (1964).Google Scholar
  10. (10).
    J. L. Osborne andA. W. Wolfendale:Proc. Phys. Soc.,84, 901 (1964); see alsoF. Ashton, Y. Kamiya, P. K. MacKeown, J. L. Osborne, J. B. M. Pattison, P. V. Ramana Murthy andA. W. Wolfendale:Proc. Phys. Soc.,87, 79 (1966).ADSCrossRefGoogle Scholar
  11. (11).
    D. H. Perkins:Int. Conf. High Energy Phenom., CERN (1961).Google Scholar
  12. (12).
    M. Csejthney-Barthy:Nuovo Cimento,32, 545 (1964).CrossRefGoogle Scholar

Copyright information

© Società Italiana di Fisica 1967

Authors and Affiliations

  • L. Briatore
    • 1
    • 2
  • M. Dardo
    • 1
    • 2
  1. 1.Gruppo Italiano di Fisica Cosmica, CNRSezione di TorinoItaly
  2. 2.Istituto di Fisica Generale dell’UniversitàTorino

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