Result of the magnetized cloud collapse for GDSPH at a resolution of 50³ particles with varying magnetic flux ratio μ going left to right from high to low. We show figures at the time of jet formation (around t = t_ff), which occurs due to the winding of the magnetic field during the collapse, which produces a magnetic tower structure. The top row shows a rendered face-on slice (L_xy = [2000 AU, 2000 AU]) of the density [g cm⁻³], the rest of the rows show rendered slices through the rotation axis (L_xz = [2000 AU, 2000 AU]), where the second shows density [g cm⁻³], the third show radial velocity [km s⁻¹], the fourth show the absolute poloidal magnetic field [μG] and the fifth shows the current density [A m⁻²], all quantities are shown in logarithmic scale. The pure hydrodynamic run (μ = ∞) of GDSPH becomes gravitationally unstable and is very similar to that of TSPH in Fig. 12. We can see that a jet is launched in the cases of μ = 75, 20, 10, 5 while in the case of μ = 2 the interchange instability (see Fig. 16) disrupts the disk before jet launching.