Poster P6: Nuclear fragmentation processes in heavy ion collisions necessary to understand propagation of cosmic rays in the Galaxy


Yuliia Balkova, University of Silesia in Katowice


Modern cosmic radiation detectors, which are placed in the Earth's orbit (such as AMS, PAMELA, DAMPE and others) allow to measure fluxes of leptons, antiprotons and atomic nuclei with accuracy of one percent in the energy range from GeV to TeV. Such accurate measurements let us to study the propagation of cosmic rays in the Galaxy and give hope to discover the effects of annihilation of dark matter.

Cosmic radiation can be classified into primary and secondary. Primordial cosmic rays are supernova remnants, while secondary cosmic rays arise in the nuclear interactions of primary cosmic rays with protons and helium in the interstellar medium. The ratio of the secondary cosmic radiation to the primary one is used to model cosmic ray diffusion in the Galaxy. The results of radiation propagation modeling make it possible to differentiate the background originating, for example, from the production of secondary antiprotons in nuclear collisions, from processes of interest, such as the production of antiprotons in the annihilation of dark matter. However, the modeling of radiation propagation strongly depends on the knowledge of the fragmentation cross-sections of the primary cosmic rays.

This work presents results on continuation of the analysis of $^{12}$C + $^{12}$C and $^{12}$C + (C$_2$H$_4$)$_n$ data taken by the NA61/SHINE collaboration. The result of the simulation analysis helps to understand the distributions obtained from the data analysis. In the same time, the comparison between simulations and data helps to find a way for treating the distributions in further data analysis. Two independent approaches are presented for the continuation of the data analysis, and their performance is verified with fragmentation elemental cross-section calculation and its comparison with world data.



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