Abstract
The dynamical evolution of a disk and the orbital migration of an embedded protoplanet are examined. We show how the migration of a protoplanet due to density waves torques can suppress the tendency for tidal truncation of the disk. A critical mass is determined as a function of the disk properties that represents the limiting mass that can sustain drift without stalling. This inertial limit is derived analytically, using a quasi-steady state theory, and confirmed by numerical experiment. This result contradicts the claim of Lin and Papaloizou that such a limit does not exist. Orbital mobility of objects due to density wave torques may have played an important role in the early evolution of the solar system.
Original language | English |
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Pages (from-to) | 490-495 |
Number of pages | 6 |
Journal | The Astrophysical Journal |
Volume | 347 |
DOIs | |
Publication status | Published - 1 Dec 1989 |
Externally published | Yes |
Keywords
- Formation-solar system
- General
- Hydrodynamics-planets