Numerical Simulation of Protoplanetary Vortices
Abstract
The fluid dynamics within a protoplanetary disk has been attracting the attention of many researchers for a few decades. Previous works include, to list only a few among many others, the well-known alpha-prescription of Shakura & Sunyaev (1973), the convective and instability study of Stone & Balbus (1996) and Hawley et al. (1999), the Rossby wave approach of Lovelace et al (1999), as well as a recent work by Klahr & Bodenheimer (2003), which attempted to identify turbulent flow within the disk. The disk is commonly understood to be a thin gas disk rotating around a central star with differential rotation (the Keplerian velocity), and the central quest remains as how the flow behavior deviates (albeit by a small amount) from a strong balance established between gravitational and centrifugal forces, transfers mass and momentum inward, and eventually forms planetesimals and planets.
Document Details
- Document Type
- Technical Report
- Publication Date
- Dec 01, 2003
- Accession Number
- ADP014794
Entities
People
- Haibo Lin
- J. A. Barranco
- P. S. Marcus
Organizations
- University of California, Berkeley