In the last decade, many works tried to explain the origin of the observed close-in Super-Earth and Sub-Neptune population using type-I migration during the protoplanetary disk phase; it is anticipated that disk-planet interaction moves them close to their host stars and the migrational effect is negated near 10-days orbit by invoking planet trap. Most works assume truncations in the protoplanetary disks caused by the host stars' magnetic field and employ sharp drop-offs in surface densities to model the truncations. In this presentation, we will show that we can construct a more realistic model by re-applying existing accretion disk model around white dwarfs to protoplanetary disks accreting onto their host star. In our model, we consider not only the host star’s magnetic field truncating the disk but also the field diffusing into the inner region of the disk. We treat both accretion heating in the disk and passive heating from the host star self-consistently. We will demonstrate that model parameters, such as magnetic-field strengths and profiles, strongly affect the migrational behavior of planets in our model, which is critical in understanding the orbital distribution of observed close-in super-Earths. A subset of our parameter is able to produce populations similar to observations.