turbulent fields. For study of chemical composition of CR (Example No. 2) various configurations (cell frequency, cell size) were used and are in detail described below. However, for directional analysis (Example No. 1) we respect the fact, that turbulent fields are common especially within spiral arms of Galaxy. Therefore we expect that 80% of volume inside spiral arm regions contain turbulent field component, while outside these arm regions only (but within surroundings of Galactic plane[^7]) 20% of total simulated volume have also nonzero turbulent field. Finally, in other outer regions of the Galaxy we suppose that only 1% of volume has also nonzero turbulent component.

As model of spiral arms we used model by [@wainscoat], which is simple four-plus-local arm model. Parameters of this particular model are in detail described in Fig. \[galarms\].

Propagation of UHECRs in GMF
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Within the next sections we describe two simple analyses of cosmic ray propagation in GMF. These analyses are done in different energy ranges and are serving for derivation of different conclusions, but they are involving the very same principles of particle motion in magnetic fields:

The propagation of the main part of UHECR (or more generally of cosmic rays) candidates (charged 