Volume 480, Number 1, March II 2008
|Page(s)||27 - 33|
|Published online||02 January 2008|
Magnetic shear-driven instability and turbulent mixing in magnetized protostellar disks
INAF – Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy e-mail: email@example.com
2 INFN, Sezione di Catania, via S. Sofia 72, 95123 Catania, Italy
3 A.F. Ioffe Institute of Physics and Technology and Isaac Newton Institute of Chile, Branch in St. Petersburg, 194021 St. Petersburg, Russia
Accepted: 5 December 2007
Context.Observations of protostellar disks indicate the presence of the magnetic field of thermal (or superthermal) strength. In such a strong magnetic field, many MHD instabilities responsible for turbulent transport of the angular momentum are suppressed.
Aims.We consider the shear-driven instability that can occur in protostellar disks even if the field is superthermal.
Methods.This instability is caused by the combined influence of shear and compressibility in a magnetized gas and can be an efficient mechanism to generate turbulence in disks.
Results.The typical growth time is of the order of several rotation periods.
Key words: accretion, accretion disks / magnetohydrodynamics (MHD) / instabilities / turbulence / stars: formation
© ESO, 2008
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.