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• W3036011000 abstract "The status of the pair-production dip as a spectral feature, produced by interaction of Ultra High Energy extragalactic protons with CMB is discussed. Greisen-Zatsepin-Kuzmin (GZK) cutoff [1] is the most spectacular prediction for Ultra High Energy Cosmic Ray (UHECR) spectrum, which status is still uncertain in the present observations. As physics is concerned, detection of the GZK cutoff means discovery of UHE proton interaction with CMB radiation. Another prediction for interaction of UHE protons with CMB is pair-production dip, the spectral feature originated from electronpositron pair production by extragalactic UHE protons propagating through CMB: p+ γCMB → p+ e + e. Originally proposed for diffuse spectrum in early work [2], this feature has been studied recently in Refs. [3, 4]. An alternative explanation of the observed pair-production dip, widely discussed now [5], was first put forward in works [6] and [7] in terms of a two-component model as the transition from galactic to extragalactic cosmic rays. Being a quite faint feature, the ee-production dip is not seen well in the naturally presented spectrum log J(E) vs. logE. The dip is more pronounced when analyzed in terms of the modification factor [2, 8], η(E) = Jp(E)/J p (E), where Jp(E) is the spectrum calculated with all energy losses included, and J p (E) is the unmodified spectrum calculated with adiabatic energy losses only. The observed modification factor is given by ηobs ∝ Jobs(E)/Eg , where Jobs(E) is the observed spectrum and γg is the exponent of the generation spectrum Qgen(Eg) ∝ E −γg g in terms of initial proton energies Eg . The pair-production dip is clearly seen in the energy-dependence of η(E) and is reliably confirmed [3, 4, 9] by observational data, as Fig. 1 shows. The comparison of the predicted dip with observational data includes only two free parameters: exponent of the power-law generation spectrum γg (the best fit corresponds to γg = 2.6 − 2.7) and normalization constant to fit the eeproduction dip to the measured flux. The number of energy bins in the different experiments is 20 22. The fit is characterized by χ/d.o.f. = 1.0−1.2 for AGASA, HiRes and Yakutsk data. For the Auger data χ/d.o.f. is larger mainly due to the low flux in the first energy bin at E ≈ 45 EeV where measurements are made with the help of surface detectors (see Fig. 1). The theoretical pair-production dip has two flattenings: one at energyEb ≈ 1×10 eV and the other at Ea ≈ 1 × 10 eV. One can see that at E < Eb the experimental modification factor, as measured by Akeno and HiRes, exceeds the theoretical modification factor. Since by definition modification factor must be less than one, this excess signals the appearance of a new component of cosmic rays at E < Eb = 1 × 10 18 eV, and thus the transition from extragalactic to galactic cosmic rays, starting at energy Eb. The second flattening automatically explains the ankle, the feature seen in all experiments starting from Haverah Park in the end of 70s. Proceedings of the 30th International Cosmic Ray Conference Rogelio Caballero, Juan Carlos D’Olivo, Gustavo Medina-Tanco, Lukas Nellen, Federico A. Sanchez, Jose F. Valdes-Galicia (eds.) Universidad Nacional Autonoma de Mexico, Mexico City, Mexico, 2008 Vol. 4 (HE part 1), pages 507–510 ID 272" @default.
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• W3036011000 date "2008-01-01" @default.
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• W3036011000 title "On the status of the dip in UHECR spectrum" @default.
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