EPJ Web of Conferences
Volume 46, 2013Instabilities and Structures in Proto-Planetary Disks
|Number of page(s)||4|
|Section||Capture and Dust Loading|
|Published online||11 April 2013|
Methods for Simulating the Heavy Core Instability
Department of Astrophysics American Museum of Natural History
Central Park West at 79th St
New York, NY
2 Department of Physics University of Wisconsin–Milwaukee 1900 E. Kenwood Blvd. Milwaukee, WI 53211 USA
a e-mail: firstname.lastname@example.org
Vortices have been proposed as the sites of planet formation, where dust collects and grows into planetesimals, the building blocks of planets. However, for very small dust particles that can be treated as a pressure-less fluid, we have recently discovered the “heavy core” instability, driven by the density gradient in the vortex. In order to understand the eventual outcome of this instability, we need to study its non-linear development. Here, we describe our ongoing work to develop highly accurate numerical models of a vortex with a density gradient embedded within a protoplanetary disk.
© Owned by the authors, published by EDP Sciences, 2013
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.