Analytic calculations of the spectra of ultra high energy cosmic ray nuclei. II. The general case of background radiation

Details Analytic calculations of the spectra of ultra high energy cosmic ray nuclei. II. The general case of background radiation Analytic calculations of the spectra of ultra high energy cosmic ray nuclei. II. The general case of background radiation

2010-06-12

arxiv.org/abs/1006.2484v1

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

The paper is the second part of a two papers series, it is composed by 18 pages and 11 eps figures

Scientific paper

We discuss the problem of ultra high energy nuclei propagation in extragalactic background radiations. The present paper is the continuation of the accompanying paper I where we have presented three new analytic methods to calculate the fluxes and spectra of Ultra High Energy Cosmic Ray (UHECR) nuclei, both primary and secondary, and secondary protons. The computation scheme in this paper is based on the analytic solution of coupled kinetic equations, which takes into account the continuous energy losses due to the expansion of the universe and pair-production, together with photo-disintegration of the nuclei. This method includes in the most natural way the production of secondary nuclei in the process of photo-disintegration of the primary nuclei during their propagation through extragalactic background radiations. In paper I, in order to present the suggested analytical schemes of calculations, we have considered only the case of the Cosmic Microwave Background (CMB) radiation, in the present paper we generalize this computation to all relevant background radiations, including infra-red (IR) and visible/ultra-violet radiations, collectively referred to as Extragalactic Background Light (EBL). The analytic solutions allow transparent physical interpretation of the obtained spectra. EBL plays an important role at intermediate energies of UHECR nuclei. The most noticeable effect of the EBL is the low-energy tail in the spectrum of secondary nuclei.

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