at least ten times more than all events detected up to now.

We use simple method to model the propagation of cosmic rays in a wide range of energy (from $10^{13}$ eV to the highest value ever detected $3.2\times10^{20}$ eV). Although our method — solution of Lorentz equation — is the simplest method of modelling of propagation of CRs, we show that it can be successfully used for wide range of different applications. The results of modelling the directional analysis of UHECR and the chemical composition of Galactic CRs are presented in this work for one complex model of GMF. In addition, we discuss experimental evidence about GMF and other GMF models and we also investigate the influence of turbulent magnetic fields.

Galactic magnetic field
=======================

Experimental evidence
---------------------

The first evidence of the existence of a Galactic magnetic field was derived from the observation of linear polarization of starlight by [@hiltner]. Many new measurements were done since then using the Zeeman spectral-line splitting (gaseous clouds, central region of the Galaxy), the optical polarization data (large-scale structures of the magnetic field in the local spiral arm) and the Faraday rotation measurements in the radio continuum emission of pulsars and of 