2D maps showing the column densities of cloud gas. Panel 1a shows the down-the-barrel (top) and transverse (bottom) projections for model R32-AL, and panel 1b shows the same for model R32-TR. The morphological differences of the cloud and filaments, associated with the different initial field configurations, in both models is evident. From left to right, the plots display column densities at t = 0.2, 1.2, 2.2 and 3.2 Myr (or t/t_cc = 0.2, 0.9, 1.7, 2.5) respectively. The morphological evolution of the cloud is highly affected by the orientation of magnetic field. Especially, in R32-TR the draping effect caused by the transverse magnetic field prevents the clouds from expanding symmetrically in the xz plane. A carbuncle effect can also be noticed in the models, so for our spectral analysis we pick sight lines at different radii from the centre.