Why don’t forming planets plunge into their stars

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Welcome, my name is Phil, and in this video I explain what stops forming planets that are migrating in a disc from plunging into their stars.
Planets don't always stay in the same orbit. There are several causes that can affect a planet's orbit and explain why exoplanets appear in certain regions. Hot Jupiter's, for example, are unable to form where we observe them because there is insufficient material in the circumstellar disc to support their growth to such massive sizes.
During the formation of a planetary system, several mechanisms work together to prevent planets from migrating inwards and plunging into their parent stars. Below are a few examples:
1. Protoplanetary Disk Dynamics
Gas Drag: In the early stages, the protoplanetary disk is filled with gas. Interactions between the planet and the gas can cause the planet to migrate. However, this migration can be halted or slowed by various factors:
Type I Migration: For smaller, Earth-sized planets, interactions with the disk's gas can lead to inward migration. However, this process can be slowed or stopped if the density and temperature gradients in the disk create regions where the migration torque changes sign.
Type II Migration: For larger, Jupiter-sized planets, the planet can open a gap in the disk. The migration then becomes coupled with the viscous evolution of the disk, which can be slower and might not always lead inward.
2. Magnetic Forces and Disk Truncation
Magnetic Fields: The magnetic field of the central star can truncate the inner edge of the protoplanetary disk. This creates a magnetospheric cavity where the magnetic pressure balances the ram pressure of the incoming gas, preventing planets from migrating closer to the star.
Magnetospheric Accretion: For young stars, material can be funneled along magnetic field lines onto the star, clearing the inner disk and creating a barrier for inward-migrating planets.
3. Photoevaporation
Stellar Radiation: High-energy radiation from the star can heat the gas in the inner regions of the protoplanetary disk, causing it to evaporate. This photoevaporation can create a pressure gradient that opposes inward migration.

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It’s at the Roche lobe overflow I realized I recognized the words but not when put together into a sentence