2001/10/24 by R. R. Rafikov, Roman Rafikov · 6 citations
Physics and Astronomy · #Angular momentum #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Inviscid flow #Planet #Planetary mass #Planetary migration #Planetary system #RADIUS #Shock (circulatory) #Shock wave #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/340228
published as Astrophys.J. 572 (2002) 566-579 · AASTeX, 31 pages, 7 figures, 1 table, submitted to ApJ
arxiv created 2001/10/24 · openalex publication_date 2002/06/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Gap formation in a gas disk triggered by disk-planet tidal interaction is considered. Density waves launched by the planet are assumed to be damped as a result of their nonlinear evolution leading to shock formation and its subsequent dissipation. As a consequence, wave angular momentum is transferred to the disk, leading to evolution of its surface density. Planetary migration is an important ingredient of the theory; effects of the planet-induced surface density perturbations on the migration speed are considered. A gap is assumed to form when a stationary solution for the surface density profile is no longer possible in the frame of reference migrating with the planet. An analytical limit on the planetary mass necessary to open a gap in an inviscid disk is derived. The critical mass turns out to be smaller than the mass M 1 for which the planetary Hill radius equals the disk scale height by a factor of at least Q 5/7 ( Q is the Toomre stability parameter), depending on the strength of the migration feedback. In viscous disks the critical planetary mass could vary from ~0.2 M 1 to M 1 , depending on the disk viscosity. This implies that a gap could be formed by a planet with mass of 2-15 M ⊕ , depending on the disk aspect ratio, viscosity, and the planet's location in the nebula.