Jupiter's migration inward in the early stages of the solar system's formation is a topic of scientific study and debate. However, the prevailing hypothesis regarding Jupiter's migration suggests that it occurred gradually over a long period.
During Jupiter's migration, it is believed that the inward movement was driven by interactions with the surrounding gas and planetesimals, which are small rocky or icy bodies. As Jupiter migrated, it created a gap in the protoplanetary disk, the swirling disk of gas and dust from which the planets formed. This gap had a significant impact on the distribution of planetesimals in the disk.
The gravitational influence of Jupiter caused the planetesimals in its vicinity to either collide with Jupiter, be scattered outward, or be captured into resonant orbits. As Jupiter migrated inward, the planetesimals were scattered and disrupted, making it difficult for them to be efficiently captured by Jupiter. Additionally, the presence of Saturn, which also formed in the early stages of the solar system, further affected the dynamics of the planetesimals.
Therefore, while Jupiter's migration did influence the distribution of asteroids and other small bodies, it did not necessarily result in sweeping up all the asteroids in its path. Some of the asteroids that were in resonant or stable orbits could have survived the migration process and ended up in the asteroid belt or other regions of the solar system. The precise details of this migration process are still an active area of research, and ongoing studies and simulations continue to refine our understanding of Jupiter's migration and its effects on the early solar system.