The movies below are from the simulations described in Collier (2018). The disks are identical at T=0. On the left shows the evolution of the disk inside the nonspinning halo. On the right the disk evolution inside the spinning halo. Two things to notice: Inside the spinning halo the bar instability happens much more quickly and after buckling the bar does not recover in this model.
Edge on view of stellar bar before and after buckling.