Analytical description of hadronic integral spectra of cosmic-ray superfamilies with Feynman scaling breaking

Abstract

We describe charged hadronic energy spectra of the cosmic-ray superfamilies named Ursa Maior and P3'-C1-890, detected by the Chacaltaya and Pamir Emulsion Chamber Collaborations, respectively, using analytical solutions for the di6'usion equations. We obtain a very good description of these events incorporating Feynman scaling breaking in the multiparticle production model of our cascading formalism. Centauro exotic events are also investigated. PACS number(s): 13.85. Tp, 96.40.De

The muon lateral distribution function as a transformation of the height-of-origin distribution in hadronic extensive air showers

“…These fluxes correspond to the one-dimensional solutions [5]. Although in [5] the production of pions from pions was neglected, the corresponding spectra exhibit similar behaviour to that shown in figure 4. Similar spectra are shown in [3, figure 6], but only for high hadron energies.…”

“…In fact, E c (X π v ) represents the characteristic pion energy for which the decay and interaction are equally probable. One can use (5) to fit the GEANT results in figure 2(b), treating E c (X π v ) as a free parameter. The function E c (X π v ) obtained from this fit (figure 3(a)) is described very well The characteristic pion energy E c (X π v ) obtained from the fit of the pion decay probability in figure 2(b) when using (5) (solid crosses), compared with (6) (the curve); and when using the approximation (11) (dashed crosses).…”

“…Using the formulae [4, equations (11), (25)] for the longitudinal nucleon F N (E, E 0 , X) and pion F π (E, E 0 , X) flux on momentum space, we present in figure 4 the calculated energy dependence of the fluxes initiated by a nucleon with an energy of E 0 = 10 15 eV. These fluxes correspond to the one-dimensional solutions [5]. Although in [5] the production of pions from pions was neglected, the corresponding spectra exhibit similar behaviour to that shown in figure 4.…”

“…The hadron and lepton fluxes in the atmosphere can be studied by means of analytical solutions of the diffusion equations that describe the cascade development. Some results [3][4][5][6][7] in this line will be discussed in section 2. We use Monte Carlo codes to calculate the muon spectra, which technique, compared with the analytical one, gives possibilities to take into account much more detail in the shower development.…”

Particle production in very-high-energy cosmic-ray emulsion chamber events: Usual and unusual events

“…We will investigate experimental data obtained in large emulsion chambers, using rigorous analytical solutions of the diffusion equations for the hadronic cascade induced by one single nucleon in the atmosphere. The one-dimensional solution F H (E, E 0 , t, t 0 ) enables us to calculate the integral energy spectrum of hadrons [14] I…”