Abstract
To answer the fundamental questions concerning the origin and nature of ultra-high energy cosmic rays (UHECRs), it is important to confront data with simulated astrophysical scenarios. These scenarios should include detailed information on particle interactions and astrophysical environments. To achieve this goal one should make use of computational tools to simulate the propagation of these particles. For this reason the CRPropa framework was developed. It allows the propagation of UHECRs with energies $\gtrsim$10$^{17}$ eV and secondary gamma rays and neutrinos. The newest version, CRPropa 3, reflects an efficient redesign of the code as well as several new features such as time dependent propagation in three dimensions, galactic magnetic field effects and improved treatment of interactions, among other enhancements.
Highlights
They are affected by the interaction of ultra-high energy cosmic rays (UHECRs) with photon fields, matter, as well as extragalactic and galactic magnetic fields
This article is organized as follows: in Sect. 2 we briefly review the photon backgrounds present in the universe and the interactions taking place at ultra-high energies; in Sect. 3 we describe the structure of the code; Sect. 4 contains short descriptions of the new features of CRPropa 3; in Sect. 5 we present some applications; and in Sect. 6 we present the concluding remarks and outlook
The simulation of UHECR propagation can be done in a one-dimensional (1D) environment, which allows the incorporation of cosmological effects such as the redshift dependence of the photon backgrounds, energy losses due to the adiabatic expansion of the universe, and source evolution, or in a three-dimensional (3D) environment, which can be used if one is interested in arrival directions, in addition to the spectrum and mass composition
Summary
The origin, nature and mechanisms of acceleration of ultra-high energy cosmic rays (UHECRs) are unanswered issues in astroparticle physics. 2 we briefly review the photon backgrounds present in the universe and the interactions taking place at ultra-high energies; in Sect. Ultra-high energy cosmic rays lose energy during their propagation to Earth mainly through four processes: pair production, pion production, photodisintegration (in the case of nuclei) and adiabatic expansion of the universe. Min 0 where is the Lorentz factor, the photon energy, σ ( ) the cross section of the nucleus-photon interaction, and max the maximum energy of the background photon, which is ∼10 meV for the CMB and ∼100 eV for the CIB. The energy loss length for photopion production, photodisintegration, pair production and adiabatic expansion of the universe are summarized, for the case of iron and proton primaries. Mass composition proton iron outside Hubble horizon energy loss processes photopion production electron pair production photodisintegration expansion of the universe all processes
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