Magnetic Cut-off of Extragalactic Protons in the Galactic Disk

Details Magnetic Cut-off of Extragalactic Protons in the Galactic Disk Magnetic Cut-off of Extragalactic Protons in the Galactic Disk

Jul 1968

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1968natur.219..355t&link_type=abstract

Nature, Volume 219, Issue 5152, pp. 355-357 (1968).

Computer Science

1

Scientific paper

ACCORDING to the results of extensive air shower experiments, as inferred from observed electron densities, the integral energy spectrum of cosmic particle radiation , where f is the combined distribution function of energy E, atomic number A and direction Ω, is of the form s-γ, with γ≅1.6 for E<~1016 eV, γ≅1.8 for ~1016 eV ~1018 eV. There is still some uncertainty about the exact position of the first knee and about the existence of the second one. If they really exist, they may be consequences of the transition from galactic to extragalactic contributions caused by the presence of a large scale ordered magnetic field in the galactic disk. The chemical composition of cosmic particle radiation, ∫dΩ f(E,A,Ω), which is well known in the low energy range, has also been the object of intensive, though still inconclusive, investigations in the high energy region E> ~1014 eV, by the measurement of the muon content1 or from the core structure of extensive air showers2 in connexion with Monte Carlo simulations of cascade development3. The amplitude of possible anisotropic contributions to the angular distribution has been found to be within the limits of statistical error, which are typically of the order of 0.1 per cent for E<~1016 eV (refs. 4 and 5), of the order of 1 per cent for ~1016 eV ~1018 eV. When studying the magnetic cut-off, the combined distribution function f'(ρ,Ω) of magnetic rigidity ρ= E/Ze and direction Ω may be considered instead of f(E,A,Ω), where Z is the charge number corresponding to A.

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