  Misalignment between rotation and magnetic field has been suggested to be one
type of physical mechanisms which can easen the effects of magnetic braking
during collapse of cloud cores leading to formation of protostellar disks.
However, its essential factors are poorly understood. Therefore, we perform a
more detailed analysis of the physics involved. We analyze existing simulation
data to measure the system torques, mass accretion rates and Toomre Q
parameters. We also examine the presence of shocks in the system. While
advective torques are generally the strongest, we find that magnetic and
gravitational torques can play substantial roles in how angular momentum is
transferred during the disk formation process. Magnetic torques can shape the
accretion flows, creating two-armed magnetized inflow spirals aligned with the
magnetic field. We find evidence of an accretion shock that is aligned
according to the spiral structure of the system. Inclusion of ambipolar
diffusion as explored in this work has shown a slight influence in the small
scale structures but not in the main morphology. We discuss potential candidate
systems where some of these phenomena could be present.
