axisymmetric quadrupole type (ASS-A) are also not completely observationally excluded yet ([@beckold]).

Poloidal and toroidal regular field components
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The dynamo model has one very interesting consequence for the propagation of CRs — namely that except of relatively flat field in the galactic disc it contains also quite strong toroidal fields above and under the galactic plane. Motions of these fields and their superpositions generate the net field in the Galaxy. The existence of such field is indirectly supported by the existence of radio thick disc mentioned above in the review of observation results. Such field could change the CR trajectories quite essentially, furthermore this type of models was not yet used for UHECR propagation simulation, therefore we decided to add these components in our simulations. We take advantage from the fact that only recently some first quantitative estimates of strengths of such fields were proposed by [@han_new].

For toroidal field we choose the model with simple geometry (circular discs above and under Galactic plane with Lorentzian profile in z-axis). For cartesian components of toroidal field it holds[^5]: $$\begin{aligned}
B_x &=& -B_T \sin(\phi)\\
B_y &=& B_T \cos(\phi)\end{aligned}$$ For the value of $B_T$ we have: $$\begin{aligned}
B_T &=& B_{max} \frac{1}{1+(\frac{z-H}{P})^2}\\
 & 