According to current theories, tidal interactions between a disk and an embedded planet may lead to the rapid migration of the protoplanet on a timescale shorter than the disk lifetime or estimated planetary formation timescales. Therefore, planets can form only if there is a mechanism to hold at least some of the cores back on their way in. Once a giant planet has assembled, there also has to be a mechanism to prevent it from migrating down to the disk center. This paper reviews the different mechanisms that have been proposed to stop or slow down migration.
- Pub Date:
- September 2003
- 8 pages, submitted for publication in 'Planetary Systems and Planets in Systems', eds. S. Udry, W. Benz and R. von Steiger (ISSI Space Sciences Series, 19, reprinted from Space Science Reviews - Kluwer)