Journal
ASTROPHYSICS AND SPACE SCIENCE
Volume 317, Issue 1-2, Pages 3-8Publisher
SPRINGER
DOI: 10.1007/s10509-008-9863-y
Keywords
Accretion, accretion disks; Hydrodynamics; Instabilities; Planetary systems: formation; Planetary systems: protoplanetary disks
Categories
Funding
- NASA [NAG5-11964, NNG 05-GN11G, NAG5-10262]
- PPARC Visitors
Ask authors/readers for more resources
Numerical hydrodynamics simulations have established that disks which are evolved under the condition of local isothermality will fragment into small dense clumps due to gravitational instabilities when the Toomre stability parameter Q is sufficiently low. Because fragmentation through disk instability has been suggested as a gas giant planet formation mechanism, it is important to understand the physics underlying this process as thoroughly as possible. In this paper, we offer analytic arguments for why, at low Q, fragments are most likely to form first at the corotation radii of growing spiral modes, and we support these arguments with results from 3D hydrodynamics simulations.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available