  Many mechanisms have been proposed to alleviate the magnetic catastrophe,
which prevents the Keplerian disk from forming inside a collapsing magnetized
core. Such propositions include inclined field and non-ideal
magnetohydrodynamics effects, and have been supported with numerical
experiments. Models have been formulated for typical disk sizes when a field
threads the rotating disk, parallel to the rotation axis, while observations at
the core scales do not seem to show evident correlation between the directions
of angular momentum and the magnetic field. In the present study, we propose a
new model that considers both vertical and horizontal fields and discuss their
effects on the protoplanetary disk size.
