Result of the magnetized cloud collapse for TSPH 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 occur due to the winding of the magnetic field during 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 TSPH becomes gravitationally unstable and is very similar to that of GDSPH in Fig. 11. We can see that TSPH does not form a jet in any of the weak field cases (μ = 75, 20, 10) and there is no sign of a magnetic tower being formed. In the case of μ = 5, we can see a jet being launched, where a current dominated magnetic tower has formed, however, the central part of the tower has been completely quenched. The μ = 2 case also launches a jet, but collapses faster than in the high resolution case, which effectively leads to easier jet formation.