field equal to $2$ mG was put into Galactic center instead of field resulting from equations above[^6]. Main motive for such arrangement was to avoid a problem with too strong field near this center ($R\sim0$) and so to keep total field strength in observed bounds and to describe character of observed filaments.

The constant $K$ was selected as follows: $K=10^5$ G$.$pc$^3$ for outer regions ($ R > 5$ kpc) and $K = 200$ G$.$pc$^3$ for central region ($R < 2$ kpc). For the intermediate region (2 kpc $< R <$ 5 kpc) we used constant absolute field strength $10^{-6}$ G. These values correspond with observed features of Galactic magnetic field: milligauss field is restricted only to the central cylinder and the vertical magnetic field is equal to $0.2$ $\mu$G in the Sun’s distance (see also Fig. \[poloidal\]).

Turbulent fields and Galactic arms
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As we pointed out above, we introduce also the influence of random fields in our simulations. Cells with characteristic size of 50 pc with random field orientation and with maximum field strength $|B|
= 10 \mu$G were added to regular, poloidal and toroidal field components.

Within two following examples we used two different approaches for introduction of 