EPJ Web of Conferences
Volume 46, 2013Instabilities and Structures in Proto-Planetary Disks
|Number of page(s)||5|
|Section||Baroclinic Instability and MRI|
|Published online||11 April 2013|
Baroclinic Instability and Vortex Amplification
1 Max-Planck Institute für
2 Jet Propulsion Laboratory - California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA
Recent years have shown that accretion disks around young stars have extended regions, which are too low ionized to couple to magnetic fields and thus the nature of the underlying turbulence cannot be exclusively magnetic. We also found that disks have in general a baroclinic density and temperature structure which means that a typical disk is radially buoyant and has a vertical velocity gradient also known as thermal wind. Here we show that the expected entropy gradients in observed accretion disks around young stars are in fact steep enough and that the thermal relaxation times are sufficiently short to allow for efficient amplification of vortices.
© 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.