2003/09/05 by Caroline Terquem, Caroline E. J. M. L. J. Terquem, Terquem, Caroline E. J. M. L. J.
Physics and Astronomy · #Astro and Planetary Science #Astrophysics (astro-ph) #Astrophysics and Star Formation Studies #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0309175
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)
arxiv created 2003/09/05 · openalex publication_date 2003/09/05 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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.